Updates to ​http://bearclaw.pas.rochester.edu/trac/astrobear/blog/martinhe11182013

Also working with A Ciardi on synthetic images.

A modification of:

​http://adsabs.harvard.edu/abs/1996ApJ...469L.127R (Rozyczka and Franco '96)

​http://adsabs.harvard.edu/abs/2000ApJ...544..336G (Garcia-Segura & Lopez 2000)

Our field is: B_toro= (R_star/x)² (x/R_star-1)*sigma. In contrast to the above authors, ours is not zero at the pole; I did not find the correct morphologies otherwise.

log(particles/cc) in colors. log(Btoroidal) contours.

Spherical wind blown bubble for NPR on Voyager poking through the heliopause.

movie 1: ​http://www.pas.rochester.edu/~martinhe/bubble1.gif

AGN jet truncation. After meeting with Eric and Alex Hubbard 2 weeks ago, we agreed on using the original magnetic tower setup to run scaled AGN sims. I've been working or resurrecting those files with the newest code revision.

Poloidal collimation. Phone call with Andrea. We discussed the dark feature at y~.4 in

​http://www.pas.rochester.edu/~martinhe/andrea/synthetic.png

real or numerical? if real, transient? I will do another run to answer this questions.

ADAM: PLEASE ANSWER JULIN'S EMAIL ABOUT A TELECON.

Met with WIlliam to do some shots for the AstroBear video.

This is my last week working 100% with you guys. Starting March the 4th, I'll only be about 4 hours a week. Sometimes in the department but reachable via email.

Continuing projects: teragrid allocation, poloidal collimation, AGN with Eric Blackman and Alex Hubbard, probably the pulsars (see below).

QUESTIONS

• what office can I use?

• should I register for the APN6 conference?, ​http://www.astroscu.unam.mx/IA/index.php?option=com_content&view=article&id=664:apnvi&catid=44:undia-alias&lang=es

-Future projects?

Disk paper referee's answers. In Adam's hands now.

Poloidal collimation. Latest run almost finished. I'll then make a synthetic map of it. Waiting for Julien to give us an update on the paper writing.

AGN jet truncation, debugging the mhd module which showed problems with the latest code revisions.

pulsar winds+GRB, potential new collaboration. Enrico Ramirez-Ruiz (from Sta. Cruz), is an expert on GRB. He and Fabio de Colle want to try to do something like ​http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:astro-ph/0610454, and then to model GRBs after glows. I'll be in touch with them and Adam as this project progresses.

Polloidal collimation.

Running the high res sim. Field lines seem to be fixed to the boundaries. However, I see spurious features which seem to develop from protections, see attachment (gray scale rim). I'm working no getting rid of this.
Found that the top part, and not the bottom —as we've been thinking—, of the lines outside the spherical wind BC (circular-ish gray region) move towards the axis, despite the fact that I'm using normal mag field BC. This needs to be fixed.

The above way of plotting the field lines is misleading. I've been playing around with the boundary conditions and with visit too.

1. killing the radial flow velocity in the bottom domain boundary introduces spurious flows.
2. the stream lines that we use to see mag fields in visit are misleading: I tried using different seed distributions in the grid to plot these lines. Some cases shows that the upper part of the lines moved towards the axis, hence giving the impression that the wind pushed the lines radially. Other seed configurations, on the other hand, showed that the bottom part of the lines were the ones moving.

So, I went back to use simple BC, where bz is forced to be parallel to both the bottom and top boundaries of the domain, and I do not touch the radial velocity at the bottom boundary. Here's a movie showing the results, descent resolutions, 2d cut (but the sim in 3d), and with log(number density) and magnetic field arrows. The fields seem to bend the way we want: stay frozen to the bottom and go around the wind. They only show a radial B component once the wind is well collimated (close to the end of the movie).

​http://www.pas.rochester.edu/~martinhe/andrea/6feb2013.gif

CRL 618 paper submitted!!!

Poloidal collimation. Running the latest sims suggested by Andrea, where the BC force field lines to remain vertical (v_r=0) at the bottom of the domain.

Lines in this sim are bent but keep their end points free. Different from previous runs (​https://clover.pas.rochester.edu/trac/astrobear/blog/poloidalCollimation)
The above set up plus fixing Bzboundary seems to show the most bent lines.

CRL618. I sent Section 4 (numerics) of the paper back to Bruce.

Poloidal Collimation. Talked to Andrea Ciardi, we discussed about new BC (more resolution, v_r=0) for the sim,

​https://clover.pas.rochester.edu/trac/astrobear/blog/poloidalCollimation

Binary disks working on Noam's corrections. Finished with all fast corrections. Missing:

• specific angular momentum
• ram pressure stripping
• impact parameter

​http://www.pas.rochester.edu/~martinhe/disk.pdf

CRL618 got comments back from Bruce, and will have a chat today or tomorrow. Paper very close to publications, he says.

Poloidal collimation, will have a skype call with Andrea soon.

Binary formed disks Will work on the referee's comments this week.

CRL 618 Wrote the "methodology, implementation and results" part of section 4 in the paper, and sent it back to Bruce. He seemed happy with the text and said he will work with it.

HELDA Did some more referee corrections (the second round !!!) to the proceedings, sent them back to the editor, and they finally got accepted.

AGN Finished the proceedings for the Milan meeting (​http://www.pas.rochester.edu/~martinhe/2012/AGNprocs.pdf), which I'll submit and post in astro-ph. Also implementing the new MHD runs.

Poloidal collimation. Waiting for Andrea's comments on the latest sim. Produced 3D renderings for the Nature paper (​https://clover.pas.rochester.edu/trac/astrobear/blog/poloidalCollimation, bottom).

Old site ​https://clover.pas.rochester.edu/trac/astrobear/blog/crl618Figures

Paper Section 4, COMPARISON TO MODEL SIMULATIONS

4.1. Models

Here we describe the methodology and implementation of our CRL618 models in detail. We have carried out two Eulerian-grid numerical simulations to follow the formation of nebular lobes via the propagation of a bullet or a jet into a stratified and ridged ambient medium. Fluid dynamics is followed in 3 dimensions using the equations of radiation hydrodynamics. The effects of optically thin cooling have been included using the cooling tables of Dalgarno & McCray (1972). The hydrodynamic equations are solved with the adaptive mesh refinement (AMR) numerical code AstroBEAR2.0 [FOOTNOTE: https://clover.pas.rochester.edu/trac/astrobear/wiki]. In particular, the Euler equations with cooling source terms are solved using a second-order MUSCL Hancock shock capturing scheme and Marquina flux functions (Cunningham et al. 2009). While AstroBEAR is able to solve the equations of magnetohydrodynamics (MHD) and to compute several microphysical processes, such as gas self-gravity and heat conduction, we do not consider these processes in the present study. The computational domain is a rectangle with dimensions 0<x<24000 AU, -4000<y,z<4000 AU. We use a coarse grid with 200x100x100 cells along with two adaptive refinement levels which increases the grid resolution by a factor of 4; the simulations attain a maximum resolution of 20 AU. Typical simulation flow times are of order 400 yr. We use BlueHive [FOOTNOTE: http://www.circ.rochester.edu/wiki/index.php/BlueHive_Cluster] and Blue Gene/P [FOOTNOTE: http://www.circ.rochester.edu/wiki/index.php/Blue_Gene/P] —IBM's parallel cluster and supercomputer, respectively— which are maintained by the Center for Integrated Research Computing of the University of Rochester. We ran simulations for about 2days, using 256 processors.

4.1.1. Initial conditions

We set the ambient medium with a static velocity (V=0) field and a density profile which decreases with distance form the origin (0,0,0) and has a series of periodic spherical ridges spaced by ~333 AU. In detail,

n_amb(r)= 300 / (r/500AU)² * .5 + SIGMA_i exp(-[6d0*{(r/500AU)-5/3-i}]²) particles / cm³,

where r is the radial distance form the origin and i is an integer number. Our choice for such structure is based on Fig. 1 of NF+07, where it is clear that the AGB “spherical halo” containing the lobes of CRL 618 has a stratified structure with semi-periodic ridges of enhanced density separated by ≈1″ (section 3). Observational studies of AGB winds suggests that they expand isotropically with mass-loss rates and velocities of order 10^-5 M_sun/yr and 20km/s, respectively (see e.g. Hrivnak et al. 1989; Bujarrabal et al. 2001). Our model AGB circumstellar medium is static, however, and we do not expect this difference to affect the results of our model because (i) we explore short, ~200yr, nebular expansion times, (ii) the axial velocity of the bullet/jet is more than an order of magnitude faster (300km/s; below) that the expected AGB wind terminal velocities.

BULLET MODEL

We base our bullet model in that of Dennis et al. (2008). At time=0 yr, a spherical bullet is placed in the grid at coordinates (r_b, 0, 0), where r_b=500AU and it is the bullet's, and the jet's, radius, with an axial velocity of 300km/s and a density profile given by

n_b (r) = min( 100*n_amb(r) , r_b²/r² ) particles / cm³.

JET MODEL

For the jet model, we continually inject gas at the grid cells which are located at the bottom face of our computational domain, within r<r_b. The injected gas has a constant axial velocity of 300km/s and a constant density of

n_j = max(n_b(r)) particles / cm³.

4.1.2. Evolution.

We present the results of our CRL 618 numerical simulations using 2d maps of density and velocity field (Figure 3, columns 1 and 3, respectively), and 1d plots of density (Figure 3, columns 2 and 4, top panel) and velocity (Figure 3, columns 2 and 4, bottom panel). All the images in Figure 3 were done using the computational data located at the middle plane of the computational doman, thus no integration of density or velocity along the line of sight was carried out.

The 2d maps in columns 1 and 3 of Figure 3 show the following structures. The bullet/jet (left/right) are the densest whitest central features. Below the bullet, or to the right of the jet (without loss of generality), we see the lobe that is formed by the bullet/jet, which is separated from the ambient medium by a contact discontinuity. Beyond the lobe we see the ambient medium which is stratified and shows a series of concentric spherical shells given by the initial conditions (above). The vertical short red, or blue, lines at the top of the maps show the positions at which the profiles in Figure 3 (columns 2 and 4) have been taken.

The bullet and the jet propagate at 300km/s, away from the ambient medium's densest region (upwards), forming an elongated lobe. We see that the expansion of the lobes is predominantly axial; the major to minor lobes' axes ratio is always > 2. We find that the lobes formed by the bullet and the jet are quite similar (compare left vs. right panels in columns 1 and 3, Figure 3), except for the material located within a bullet/jet radii from the axis. As the bullet (jet) penetrates the ambient's shells, these form regularly separated vertebrae-looking features along the lobe. The axial velocity of these features decreases with radial distance from the axis.

We see that the bullet shrinks as it propagates though the ambient medium (compare columns 1 and 3, Figure 3). Similarly, the head of the jet seems to adopt a conical up-ward pointing geometry as it propagates. Such effect is due to ablation of the material located at the working surface of the bullet/jet as it interacts with the ambient medium. Such effect is consisten with the models of Dennis et al. (2008).

The density profiles in Figure 3 (columns 2 and 4, top panel) show the following.

the evolution of the bullet and the jet quantitatively, as a function of time and position inside the lobes.

Fig. 3. Models of a bullet and jet with outflow speeds of 300 km s–1 propagating through an AGB wind with periodic density ridges spaced by 333 AU after 100 y (left half) and 200y (right half). The grey-scale panels show the density distribution and the streamlines in the midplane for bullets (left half) and jets (right half). The associated densities and radial velocities along lines in the midplane on or displaced from the symmetry axes are plotted to the right of each of the grey-scale images. The offsets are labeled and indicted by vertical tics along the top of each grey-scale image.
Fig 4. Predicted position-velocity diagrams of bullets (left panels) and jets (right panels) at times t = 100y and 200y integrated over a slit. Slit widths are indicated on magnified 3-D model projections of the fingertips (insets). The symmetry axes of the P-V diagrams are inclined by 30o to the plane of the sky. The grey scales are proportional to the surface brightness computed from the square of the density. Note that the bow shocks and their trailing wings—but not the lateral edges of the fingers—are visible in HST images through emission-line filters (cf. Fig. 5). Thus observed P-V diagrams are composed of (1) a tilted line connecting the nucleus and bow shock and (2) a second line left of the bow shock.
Fig 5. Bullet and jet model simulations (midplane) at 100y compared to the eastern fingers of CRL618. [NII] emission is primarily intrinsic whereas other filters become dominated by scattered stellar light to the left of the fingertips.

Bruce's wish: that Martin/Adam explain why the speeds of the gas in the body of the lobes follow a Hubble-like pattern since Bruce makes the case in section 5 that this is where the H_2 emission is likely to arise.

Matt, Winglee & Bohm, 2003, MNRAS, 345, 660, ​http://adsabs.harvard.edu/abs/2003MNRAS.345..660M

Spruit, H.~C., Foglizzo, T., & Stehle, R., 1997, mnras, 288, 333 ​http://adsabs.harvard.edu/abs/1997MNRAS.288..333S

19 dec '12

3D rendering with color magnetic field lines and grey density iso-surfaces. This is an axial cut of the numerical domain which shows the inner structure of the outflow and the geometry of the mag. field lines. For this run, the field lines' foot points are continually kept fixed at the bottom of the computational domain, and better resolution has been used. The collimation seems weaker than in previous runs (below), even though the same parameters (image above) were used.

18 dec '12

Ditto but for the run of Nov. 21

CRL 618, new data and plots @ top of ​https://clover.pas.rochester.edu/trac/astrobear/blog/crl618Figures

Binary disks paper. Working on Noam's comments.

CLR 618.

• New plots: ​https://clover.pas.rochester.edu/trac/astrobear/blog/crl618Figures
• Writing "numerics" section of the paper.

PN jet power. Helping Scott to run PN jets. He's already running in grass and playing with module parameters. Movies/images soon.

AGN.

• New data: ​http://www.pas.rochester.edu/~martinhe/2012/agnTrunc.pdf
• Writing Milan's proceedings and running sims.

CRL 618

Movies:

Clump: ​http://www.pas.rochester.edu/~martinhe/2012/crl20nov.gif

TOKES ?

CRL 618

Jet sim running.	New clump sim running

AGB r^-2 radiation pressure force

Running tests on the global binary sims, i.e. 2 stars in the grid, 40 AU.

We talked about including a A* r^-2 force term to the momentum equation to account for the wind's acceleration region. We need to decide on the strength of A.

the mom equation is:

v dv/dr = - 1/rho dp/dr - G m r^-2+A r^-2…(1)

it's useful to consider the relative forces: Gamma = A/Gm. So far we've used Gamma=1, but we want 0<Gamma<1.

Up: wind velocity / Mach. Bottom: wind density. VS. distance and Gamma values from Intro. to stellar winds, Lamers & Cassinelli.

Polodial magnetic collimation

Andrea: On the inside your flows look much more like the laboratory ones, here is an image from your simulations (colour map is density, vector is velocity, and lines is magnetic field lines).

AGN jet trucnation

Dark spot in the weak AGN radio jet survives for 30kyr when the red giant crosses its axis!

Poloidal collimation New run finished. Andrea's looking at the data. New runs to be ran soon.

AGN jet truncation Run with the star at the jet's axis is running:

CRL 618, new run (v_clump=250km/s, higher densities [stringer cooling]) running in Bgene:

Binary. Debugging old module to use the golden version.

hedal procs writing answers.

AGN jet truncation. Data with the desired resolution:

Now running the long term evolution of this run and the on-axis version.

Kraken. Waiting for reply from teragrid on the tokens.

CRL 618. Phone call with Bruce. The numerical section of the paper is in our hands. He thinks that the other sections of the paper are in very good shape. New runs:

• v_j=200km/s with higher dens_j and dens_amb to produce thinner lobes. I addition, we will add a tracer field that follows the onion-like density distribution of the ambient, to see if molecular H in the ambient can get "glued" to the lobes. This is motivated by the effect that the ambient rings have on the structure of the lobes:

.

Global binary sims (the 2 stars in the grid). Test runs have begun.

Poloidal magnetic collimation. Still working on getting the parameters that we want.

PN luminosities vs. Mdot. Met with Eric B. and chatted about his student, Scott, and the project about PN jets with different Mdots. Will meet with Scott this week.

Poloidal collimation.. Running a set of sims to match the morphology of the latest Andrea's experiments.

AGN jet truncation. Running the hydro cases with the newest resolution.

Binary global simulations. Started implementation using the golden version of the code.

Disk paper. In Jason's hands now. Aim to submit by Friday.

CRL618. Emails with Bruce. He plans to send us a draft of the paper (or at least the theory section of it) by weeks end.

Will give a talk at RIT this Thursday.

• Disk formation in binaries. The shape of the stagnation point. Images from the 15AU case. CLICK TO ENLARGE.

Vel. streamlines that start close to the grid boundaries and finish (most of them) in the disk. Black is fast and white is slow.	Pole-on view	Perspective view
Iso-surfaces. Blue=disk; red=low vel gas.
One white vel streamline that starts at the boundary, gets to the stagnation point and is accreted then. Velocity field in colors in the vicinities of the stagnation region.

My conclusion form these plots is that the stagnation occurs at a surface with a complex shape; not a point. Lets call this the stagnation region. An improved version of these images has been added to the paper.

• Poloidal collimation of isotropic winds. Phone call with Andrea. He has new unpublished experimental data in magnetic field strengths never explores before. He has simulations of the experiments which agree quite well. Wants me to find astro parameters which will match the morphology and shock structure they see. Also, to connect the experiments and their sim, with our astro sims and thus astro observations.

AGN jet truncation

• The x-ray Italy conference went well. We may have gotten another astrobear user, a phd student from Bologna who's simulating disks using Zeus-2d, and a lady from Grenoble France who was very interested in our models of AGN jets, so a potential collaboration.
• Will resume running these simulations this week.

Disk paper Almost done with my corrections. Extending the disk material orbits section. Will give the final version to Adam early this week. I believe is almost ready for submission.

crl 618. Exchangins emails with Bruce about previous sims on the object. He's working on the paper and will send it to us in some weeks time.

Flipping Disks. Plan to set the 1st test for the flipping disks interacting with stellar winds.

Collimation of isotropic winds In correspondance with Andrea Ciardi about his nature publication.

teragrid Getting the tokens to acces kraken.

Will give a talk on magnetic towers and disk at the CIRC symposium this Friday.

Also preparing job applications.

AGN jet/Stellar wind interaction. I have new data from 2 runs: weak and strong jet. The stellar wind now has a mass loss rate of 10^-4M_sun/yr and it goes off at the jet's axis. The wind lasts for 10kyr only, and after that I stop injecting it.

Jet tracer maps. It's a time sequence (bottom of each map) from left to right. Next to each other you see the with-star vs. the without-star sims, left and right, resp. You can see that the effect of ONE star on the jet lasts for 40kyr.
The same is true for the kinetic energy: snapshot at 30kyr after the star was ejecting its wind.

The effect is much milder when the AGN jet is stronger. This is a logarithmic density map with overlaid jet tracer contours.

Disks. Status of the paper?

AGN jet truncation. Progress on the poster. New sims look more realistic and are half way done:

Here you see the star half way though the jet's beam (red). The star's wind injection radius is about .125-.25 jet radii (it was ~1 jet radius before). Cocoon material is blue. This is a logarithmic color map of the jet's tracer field.

Here's a log dens movie of the sim: ​http://www.pas.rochester.edu/~martinhe/2012/17sep12.gif

Waiting for Andrea and Bruce to respond for the wind collimation and CRL 618 projects.

• AGN jet truncation. Running the simulations and preparing the poster for the Italy conference. The wind radius that we used in the last runs was too large to be realistic, but they gave us some data to work with. I'm now running sims which will likely be production runs.

• Magnetic collimation of spherical winds. Andrea and I will have a phone call meeting early this week to discus future runs on this project.

• Sent HEDLA proceedings to arxiv and updated title of the magnetic tower paper.

• Writing research proposals for job applications.

• Disks. Any news on the paper plan?,

• Teragrid large proposal. No news from them yet,

• AGN jet truncation. Got all conference travel arrangements done, working on the poster

(​http://www.pas.rochester.edu/~martinhe/2012/AGNposter.pdf) and running the sims.

Seems I need reruns with smaller RG wind radii, see ​http://www.pas.rochester.edu/~martinhe/2012/4sep12.gif, where I show 3 planes perpendicular to the RG orbital trajectory to follow the RG mass-loading on the jet.

• Mag. tower paper. Solved all publishing matters, so it's is press now,

• Spherical wind collimation via a uniform mag. field (Ciardi). Last run (​http://www.pas.rochester.edu/~martinhe/2012/andrea6aug12.gif) was not cooling. Running a cooling version of it at Bgene now:

​http://www.pas.rochester.edu/~martinhe/2012/5sep12.gif

Will email Andrea once I get the data,

• Colloquium at AI-UNAM. Went really well, got good feedback, a potential permanent position for the future and this interesting reference on non-magnetized jet launch models: ​http://adsabs.harvard.edu/abs/2011arXiv1103.0250H.

• Magnetic tower paper accepted in ApJ!'''

• Spherical wind against constant vertical mag fields (from HELDA). 1st test with revision 951 ran well in Bgene: completed in 28hrs with 256 procs. ​http://www.pas.rochester.edu/~martinhe/2012/andrea6aug12.gif

Noticed quite a bit of protections in jets runs (AGN and the above ones) using a grid boundary in r951, which I didn't see before.

• Binary disks. 15au run added to the paper, but its disk outer radius -formed by light gas- is larger than the 10au case (paper Figure 4). Running 10au case with 4amr and latest module to make sure the disk sizes we're getting are physical. Added more text into the paper, will hand it to Jason next week while I'm in Mex. draft:

​http://www.pas.rochester.edu/~martinhe/2012/binary/paper2.pdf

• AGN jet traction by AGB winds. 3 HD sims are running (strong jet with AGB trajectories that cross both the jet's edge and axis; weak jet with AGB trajectory that crosses the jet's edge) with the latest revision and in Bgene/Bhive.

• Off to Mexico City from the 13th of Aug to the Sept. the 1st for US visa renewal.

• Adam: I need a recommendation letter for the Marie Curie Fellowship by Aug the 15th please.

Disks

• 15 AU run up to 2.5 orbits. Consisten results with the 10 and 20 AU sims, however, for some reason that I have yet to understand, the Disk mass and particle accretion profiles show more variations than the other two cases:

	Disk mass
	particle accretion

• paper. Added more and info and still writing the results and intro sections, see updated DRAFT at ​http://www.pas.rochester.edu/~martinhe/2012/binary/paper.pdf

-AGN jet truncation. Sims showing quite a bit of protections which lead to jet asymmetries. Working on solving this.

• Improving figures and writing the results section of the disk paper. Latest draft: ​http://www.pas.rochester.edu/~martinhe/adam/paper.pdf
• Pushing the 15AU sim in bluehive and bgene (very sow), close to 2 orbits.
• Pushing the AGN sims.
• Writing job application research proposals.

Binary

New 10 AU disk mass plot shown along with mass flux out of the grid. The gradients are consistent: the disk mass decreases as the outwards mass flux increases. Thus during the first 3 disk orbits the wind removes a few 10% of the disk mass. It also makes sense that the effect is less significant in the 20 AU case (below); the disk is father away from the primary hence its wind has less ram pressure, by a factor of r-1.
New 20 AU disk mass plot shown along with mass flux out of the grid. The gradients are also consistent.
New 20 AU angular momentum profiles vs disk radius and time. Trying to understand whether these plots are correct and if they tell us something about warping. There are 10 data points per orbit and per coordinate. The momenta are added on spherical shells centered at the secondary. Though our 20 AU disk is far from Keplerian, as shown by the streamline maps, jzKeplerian ~ r½. The 1, 2 and 3 orbit jz profiles (black ones, left panel) are proportional to r~.9.

• 15 AU sim running again, up to .5 orbits and the disk has formed already. Should have the data by next week.

Teragrid proposal and magnetic tower paper submitted.

AGN jet truncation trying to get runs finished. May have some movies here by Tuesday the 17th.

Ranger resources almost finished. Kraken ans Steele queues are insanely long.

Binary

• New paper figures, No. 5, 6, 7, 8 and 9: ​https://clover.pas.rochester.edu/trac/astrobear/blog/martinhe06202012

• 15 AU, forms a disk since .3 orbits.

• Disk flow streamline movies:
  • 10 AU ​http://www.pas.rochester.edu/~martinhe/2012/binary/10lines2.gif
  • 20 AU ​http://www.pas.rochester.edu/~martinhe/2012/binary/20lines2.gif
  • Note the eccentricity differences.

Disks

15au and 30au cases running.

Movies of (3d) radial inward mass flux density, $\vec{p} \cdot -\hat{r} = -(x\,p_x+y p_y+z\,p_z)/|r|$, where $\vec{p}$ is the linear momentum vector. The red material accretes while blue one goes away from the particle. Polar accretion does not dominate the toroidal+radial one.

Note that the color scale on the right is smaller than that on the left to stress gradients.

• 10au case ​http://www.pas.rochester.edu/~martinhe/2012/binary/10radFlux.gif
  • 3d view of the above ​http://www.pas.rochester.edu/~martinhe/2012/binary/10radFlux3d.gif
• 20au case ​http://www.pas.rochester.edu/~martinhe/2012/binary/20radFlux.gif
  • 3d view of the above ​http://www.pas.rochester.edu/~martinhe/2012/binary/20radFlux3d.gif

Paper figures page: ​https://clover.pas.rochester.edu/trac/astrobear/blog/martinhe06202012

New cool movie from the 10 au case (the stupid arrow should be ~1 inch to the left): ​http://www.pas.rochester.edu/~martinhe/2012/binary/10au-3dDisk.gif

To do list form the meeting on June 21.

1. Confirm we have a disk in the 20au case by comparing the disk's radial velocity profile vs a keplerian one.

2. State in the paper that we are not far (far) from the WRLOF limit in the 10au (20au) cases, and refer to
   • Mohamed-Podsiadlowski, ​http://adsabs.harvard.edu/abs/2011ASPC..445..355M)
   • Sandin, ​http://adsabs.harvard.edu/abs/2008MNRAS.385..215S

3. Assess the numerical viscosity in our sims by comparing current 10 and 20 au sims with different effective resolutions

10AU case. Not significant difference once steady.

4. Analyze the accretion that we find with
   • profiles of radial mass flux on a longitudinal plane, vs polar angle and time
   • 2d maps of radial mass flux on the orbital plane vs time
   • compare profiles of Mdot vs time for 10au sims with
     • orbital motion (exiting data)
     • no orbital motion (new quick run)

5. Runs
   • keep running current 20au
   • start running a 15 au
   • start running a 30 au

IN NO PARTICULAR ORDER

1. 10au accretion rate evo. Still higher than expected. val-borro et al. table3, report $\dot{M}_{acc}/\dot{M}_{wind} \sim$0.06 after 2 orbits for a 70AU case. The {\bf gradients} in the corresponding accretion rate evo profile (their fig. 12) are similar to ours; a very fast and brief initial increase followed by rather mild variations.
2. 20au accretion rate evo.
3. 10au Disk mass evo.
4. 20au Disk mass evo.
5. 10 au, disk density structure at 4 times, orbital plane view. The disk is consistently asymmetric. By time=.1 orb it has a width of about 1.5 AU. By time=1orb, the disk radius increases 4-fold and its morphology changes mildly. Density gradients are steeper in the disk part that faces the incoming wind.
6. 10 au, disk density structure at 4 times, longitudinal plane view. The disk has a flared structure.
7. 20 au, disk density structure at 4 times, orbital plane view.
8. 20 au, disk density structure at 4 times, longitudinal plane view.
9. 10 au (black) vs. 20 au (red), disk orbit streamlines comparison at 3 times: 1orb=thin; 2orb=thicker; 3orb=thickest, orbital plane view. Grid squares are 1 AU2.

Binaries

• 20au. New run has produced a disk. Still running and consistent with previous lower res run (see 20au run in table below). The new one: 64x64x32+4amr @ ranger (Baowei's), 512p, ~.25 orbits/day. MOVIE: ​http://www.pas.rochester.edu/~martinhe/2011/binary/18jun2012.gif.

This run produced sensible particle accretion rates:

Ranger is very friendly, e.g. consistent access to 64-512procs for 1 day with a queue wait time of <~ 30min. I suggest we apply for more time there soon.

-10au. New run with the same resolution as the above one, is running in ranger. Aim to see whether this 10au run produces lower particle accretion rates; I found higher values than the expected ones, for factors of ~30, for the 10au run in the table below.

-paper. The model/setup/IC sections are almost ready. I've been writing some of the 10au results. Missing: intro, more about the 10au results, the 20au results, some discussion and conclusions.

Disks

-20au preliminary early evo test with more resolution than before, ​http://www.pas.rochester.edu/~martinhe/2011/binary/20au-1000k-64x64x32-4amr-correctWINDdens.gif. This sim has a resolution of 64x64x32+3amr. AGB wind inflow enters the -x, +y and +-z boundaries. Improved versions of this sim should run in kraken soon.

• 10au. Evo plots:
  • NEW
  • OLD: ​http://www.pas.rochester.edu/~martinhe/plot.pdf, these are the disk mass and the particle accretion rate, red and green respectively. Mdot (green) is higher than expected for an AGB mass-loss rate of 10^-5M_oyr^-1, however, I found a mismatch between the wind's density at the position of the grid's inflow boundaries, relative to the primary's position. Thus the injected mass-loss is actually 3x10^-4M_oyr^-1. With this in mind, a Mdot_particle ~ 4x10^-6M_oyr^-1 (green profile) is sensible. I'm running a 10au and a 20au (with more res) versions, with a corrected mass-loss of 10^-5M_oyr^-1. I can already see a lower Mdot_particle for the 10au case.
• Here's the very preliminary paper's draft. A LOT is needed still, ​http://www.pas.rochester.edu/~martinhe/2011/binary/draft1.pdf

• Opened a ticket about the code's efficiency: ​https://clover.pas.rochester.edu/trac/astrobear/ticket/218. This is slowing down the co-rotating disks research.

• Progress in kraken (managed to run for ~8hrs on 4092p), but issues too, see tickets 209 and 217. Will try the latest rev.

• The code is behaving well in steele, but queues are very, very busy.

Towers. Working on the ApJ referee's comments on the paper.

AGN jet truncation by red giant stellar winds. Latest sim ​http://www.pas.rochester.edu/~martinhe/2011/agn/hd-strongJet-edge2.gif shows that the red giant's (RG) wind, which crosses the edge of the jet's beam, strongly affects the collimation of the AGN jet. Note that in the previous sim (​http://www.pas.rochester.edu/~martinhe/2011/agn-6apr-dens2.gif) the RG's orbital path intersected the jet's axis, affecting the jet's beam more drastically.

-Biaries. Writing the setup and results section of the paper. 10au (​http://www.pas.rochester.edu/~martinhe/2011/binary/4panels-10may12B.gif) and 20au (​http://www.pas.rochester.edu/~martinhe/2011/binary/4panels-14may12a.gif) sims continue to run, time > 2 orbits, in Bhive. 20au runs with 6 time more res (as discussed last friday) are in the queues of kraken and steele, both of which are quite busy.

-Magnetic tower. Finished hedla proceedings and waiting for co-authors comments. Doing the ApJ's referee's corrections.

-AGN jet truncation. Have a reservation in Bgene today to figure out why the code is not working in that cluster. I'll then continue with the AGN runs (which I was doing in Bhive but I'm now using it for the binary runs.).

• Perets & Kenyon's (pk, semi-analytic, ​http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1203.2918):
• Val-Borro et al. '09 (vb, 2D flash, ​http://adsabs.harvard.edu/abs/2009ApJ...700.1148D)
• M&M '98 (SPH, ​http://adsabs.harvard.edu/abs/1998ApJ...497..303M)
• see others at ​https://clover.pas.rochester.edu/trac/astrobear/blog/Binary%20papers

6 June '12, 10 AU case, Mdot_primary=10^-5M_o yr^-1

	Disk mass evolution. Compare with pk model 2, fig. 1 top, but note that qpk=3 while qus=1.5. I'll soon have a similar plot for the 20 AU case which should be compared with M&M figure 5 bottom; M&M see an increasing disk mass with a final value of 5x10-6 Mo yr-1.
	Evolution of the mass accretion rate onto the particle. The converging value of ~5x10-6 seems a factor of 50 higher than expected. Comparing with table 3 M&M, models 1 and 2: MdotM&M~.9-3x10-6 ; Mdotus~5x10-6, so we seem to be off for a factor of order 1.6-5.6. Comparing with pk model 2, fig. 1 bottom, (but note that qpk=3 while qus=1.5) we are off by a factor of ~30. Investigating further.

-20au preliminary early evo test with more resolution than before, ​http://www.pas.rochester.edu/~martinhe/2011/binary/20au-1000k-64x64x32-4amr-correctWINDdens.gif. This sim has a resolution of 64x64x32+3amr. AGB wind inflow enters the -x, +y and +-z boundaries. Improved versions of this sim are running in ranger and queued in kraken.

• vel_w=10km/s
• temp_w=1000K
• m_prim=1 M_o
• m_sec = .5 M_o
• resolution= 63³ cells + 2 particle refinements
• r_Bondi= G m_sec / (vel_w² + vel_orb-second²)
• l_grid = 2.5r_Bondi
• r_soft = 4 cells

Inflow form the top, bottom, lower Y and larger X is killed.

^a No. density log grey scale [cu] + color velocity [Mach]. Top left, top right, bottom left and bottom right show the entire orbital plane, a zoom into the orbital plane, the entire longitudinal plane for a phi angle parallel to the wind at the origin, and a zoom into the longitudinal plane, respectively.

^c ​https://clover.pas.rochester.edu/trac/astrobear/ticket/209#trac-add-comment

Co-rotating binary sims: ​https://clover.pas.rochester.edu/trac/astrobear/blog/martinhe04232012

PN paper re-submitted to mnras after addressing the referee's comments. Eric has seen it too. Here's the new paper: ​http://www.pas.rochester.edu/~martinhe/paper.pdf

AGN jet truncation. MHD tests going well. Found parameters for a PFD jet and I'm running the last tests on it. Already seen that the RG wind creates a hydro island round the jet due to flux freezing.

CRL618. Reading some references sent by Bruce, which may be included in the paper. He's preparing a draft.

PFD vs MCL jet. The long adiabatic mag tower simulation is in the queue at bgene.

CIRC poster session this Friday, presenting the mag tower.

The simulations in this blog are based on these ideas:

⁺​https://clover.pas.rochester.edu/trac/astrobear/blog/johannjc04032012

⁺⁺​https://clover.pas.rochester.edu/trac/astrobear/blog/johannjc03312012

8May '12

• 30AU, r_Bondi=6, vel_w=10km/s, t_w=1000K, \gamma=1 with 96x96x144 + 2amr res, 4hrs, 40 afrank procs, bhive

• 30AU, t_w=1000K, \gamma=1 with 100x100x160 + 4amr res. No disk formed after .07 orbits (3days, 1024 ranger procs).
  • Movies of logarithmic density (grayscale)and linear velocity [Mach]:
    • orbital plane ​http://www.pas.rochester.edu/~martinhe/2011/binary/30au-1000k.gif
    • orbital plane, zoom in ​http://www.pas.rochester.edu/~martinhe/2011/binary/30au-1000k-z.gif
    • longitudinal plane, zoom in ​http://www.pas.rochester.edu/~martinhe/2011/binary/30au-1000k-z-l.gif

27 Apr '12

• 40AU, t_w=3000K, \gamma=1 with 168³ + 4amr res is running at ranger's long (1024p, 2days) queue.

• 10AU, t_w=3000K, \gamma=1 with 112x144x160 + 3amr res. No disk formed after .21 orbits.

Orbital plane	Longitudinal plane

• Understanding/solving the dynamics of the 40au, \gamma=1.1, t_w=300K sim (below).
  • Here's a temperature map of the whole orbital plane ​http://www.pas.rochester.edu/~martinhe/2011/binary/corot-40au-sol2-300K-gamma1.1e.gif.
    • Hot gas (10⁵ K) seem to discontinually emanate from the particle, specially early in the sim.
  • Now running a short test, same parameters, with 10 times more frames.
    • Temperature movie 2. 20 times faster frame rate than the temp movie above and zoomed in to the particle, ​http://www.pas.rochester.edu/~martinhe/2011/binary/corot-40au-sol2-300K-gamma1.1f.gif.

26 Apr '12

• 10AU, t_w=3000K, \gamma=1 with ~64³ + 2amr. No disk formed after 2 orbits (16hrs, 256 ranger procs). Trying 2 times more res.

• 40AU, t_w=3000K, \gamma=1 with ~128³ + 2amr. No disk formed after .44 orbits (1day 256 ranger procs). Images show a zoom in to the particle.

Orbital plane	Longitudinal plane

• 40AU, t_w=300K, ideal gas solver, \gamma=1.1. Very interesting dynamics.
  • ~128³+2amr, 0.2 orbits / 1day, 256 ranger procs.
  • Movies of logarithmic density (grayscale)and linear velocity [Mach]:
    • orbital plane ​http://www.pas.rochester.edu/~martinhe/2011/binary/corot-40au-sol2-300K-gamma1.1a.gif
    • orbital plane, zoom in ​http://www.pas.rochester.edu/~martinhe/2011/binary/corot-40au-sol2-300K-gamma1.1b.gif
    • longitudinal plane ​http://www.pas.rochester.edu/~martinhe/2011/binary/corot-40au-sol2-300K-gamma1.1c.gif
    • longitudinal plane, zoom in ​http://www.pas.rochester.edu/~martinhe/2011/binary/corot-40au-sol2-300K-gamma1.1d.gif
    • Jet? This corresponds to the last frame of this short test sim.

Though I was expecting differences between the \gamma=1 and \gamma=1.1 cases, I'm surprised that they are SO different. This is inconsistent with ​http://adsabs.harvard.edu/abs/2000MNRAS.316..906M. One has to be careful though for their parameters are in general different than ours.

24 Apr '12. Research meeting. To try:

• 10AU and 40AU low res and t_wind=3000K, instead of 300K. Tests ran
• 40AU, t_wind=300K, ideal gas solver, \gamma=1.1. short test ran
• Jonathan's latest thread implementation on the global (2 particle) sims.

23 Apr '12

• separation = 40AU
• m_prim= 1.5 M_o
• m_sec = 1 M_o
• temp_w = 300 K
• dens_w = 1.5x10¹¹ gr/cc
• v_w = 15 km/s = 15 Mach
• v_orbit-sec = 4.5 km/s
• r_Bondi = Gm_sec/ ( v_w² + v_orbit-sec² )= 3.6 AU
• r_soft = 4 cells
• r_Bondi/r_soft = 19.3
• r_orbit/r_Bondi = 6.62

A) low res=56x72x80 + 3 particle Ref. .43 orbits / 26 hrs with ~ 32 afrank nodes in bhive. Running.

Movies:

• dens+vels, ​http://www.pas.rochester.edu/~martinhe/2011/binary/corot-40au-sol2.gif

• dens+vels, secondary zoom in, ​http://www.pas.rochester.edu/~martinhe/2011/binary/corot-40au-sol2z.gif
• dens+vels, secondary zoom in, longitudinal plane ​http://www.pas.rochester.edu/~martinhe/2011/binary/corot-40au-sol2l.gif

Tilt?. At some point during this simulation I see a rather brief (lasting for ~ 0.005 orbits) tilted disk-like structure similar to the ones I saw in the global (2 particles) sims (​https://clover.pas.rochester.edu/trac/astrobear/blog/binaryBondi, top table).

B) high res= 56x72x80 + 5 particle Ref. .05 orbits / 20 hrs with 256 ranger procs. Running. Note the images below show gas at a point at which the mass of the secondary is increasing to reach its final 1M_o value. This was dome for numerical stabilization and, given that we want to run the sim for several orbits, it should not affect the formation/evolution of the disk.

Gas momenta. I'm using this plot trying to understand why gas is not going about the seconday as expected.

20 Apr '12

We've determined that Jonathan's module template does not have a frame/secondary which follow a circular orbit and has extreme parameters. Presumably, a disk is formed in such setup, with a separation as large as 350AU, because the unstable orbit is subject to a lot shear from the flow which might make rotation about the secondary easier.

The 1st, intermediate-res test with the full wind solution (wind+secondary's gravity) has completed for

• separation = 10AU
• m_prim= 1.5 M_o
• m_sec = 1 M_o
• temp_w = 300 K
• dens_w = 1.5x10¹¹ gr/cc
• v_w = 15 km/s = 15 Mach
• v_orbit-sec = 8.9 km/s
• r_Bondi = Gm_sec/v_w² = 4 AU
• r_soft = 4 cells
• r_Bondi/r_soft = 21
• r_orbit/r_Bondi = 1.52
• running time ~ 1 orbit/11hrs (16afrank, bhive nodes)

Movies:

• dens+vels, ​http://www.pas.rochester.edu/~martinhe/2011/binary/corot-10au1.gif
• dens+vels, secondary zoom in, ​http://www.pas.rochester.edu/~martinhe/2011/binary/corot-10au2.gif
• ram pressure, zoom in, ​http://www.pas.rochester.edu/~martinhe/2011/binary/corot-10au3.gif

Higher res test running now. Note that we've not used this (new) wind solution for the 40AU case.

19 Apr '12 Trying to understand why Jonathan's setup⁺ forms a disk while mine (below) doesn't. Here's a parameter comparison.

^a \dot{M} = \rho 4 \pi r_{sec}^2 v_w. \text{~Thus using~} \rho=1 ~~\text{part/cc and~} r_{sec}= 50 \text{~AU (the position of the grid boundary), yield}

\dot{M}=1.7 \times 10^{-14} M_o / yr << \dot{M}_{AGB} \sim 1 \times 10^{-5} M_o/yr.

^b \text{~From~} m_{pri}/(m_{pri}+m_{sec}) \sqrt{G(m_{pri}+m_{sec})/a}, \text{~where~} a \text{~is the stellar separation.~}

^c \Omega r = 2*3=6 \text{~cu~} = .54 \text{~km/s~}.

The combined mass and the separation in the run of the left column seem extreme.

16 Apr '12

Same parameters as the run below, but a slightly larger grid and 3 spatially fixed refinement (particle) levels, ​http://www.pas.rochester.edu/~martinhe/2011/binary/corot1.gif.

• Discussion and further analysis needed.
• I do not see a disk forming. Will try with 2 more refinements in order to have ~ 40cells/r_Bondi.
• The flow shows some strange pulsations not related to protections.
• The accretion tail is not a collimated one, like that in the low res run (below), and it broadens up.

6 Apr '12

I've got Jonathan's new co-rotating frame setup^+,++ running for a binary system with the parameters below which are representative of my previous lab frame binary runs (see the table below):

• Temp_wind=300K
• AGB mass-loss = 10^-5 M_o yr^-1
• vel_wind=9 km/s (as in Mastrodemos & Morris)
• vel_wind/vel_orbit_sec = 2.01
• a=40AU
• circular orbit
• q=m_pri/m_sec=1.5
• r_soft=4 cells
• 64x64x128 cells, fixed⁺⁺⁺
• grid: 40x40x80 AU.
• t_run~.5 orbit/hr in 16 debug bluehive procs
• dx_co-rotating ~ 13 dx_{lab frame}

Running in Ranger's normal queue, 1024procs for 2 days.

Binary. Jonathan and I have completed the implementation of the full wind solution for the co-rotating frame. The one we used before was not including the secondary's gravity. See more updates at ​https://clover.pas.rochester.edu/trac/astrobear/blog/martinhe04232012

Magnetic tower.

• I did a little presentation in a workshop organized by Dan and Manoj last weekend. They are quite interested in our magnetic tower/cooling jet models to explain some of their recent observations.

• Off to Florida on Sunday for HEDLA12.

AGN jet truncation.

• I've registered to the x-ray conference (​http://www.brera.inaf.it/xrayastronomy_anniversary/).
• Time to add magnetic fields to the AGN jet and think about production runs.

More info (images) soon.

-Running in ranger (teragrid)! Limited to 2hrs in 256 procs. though; only the development queue has the updated libraries necessary to run the code.

-Binary.

• Co-rotating frame, new sim with more resolution, ​https://clover.pas.rochester.edu/trac/astrobear/blog/binaryBondi
• Testing a new wind solution, one that includes the secondary's gravity.

-AGN jet truncation. The RG has crossed the AGN jet's path, ​http://www.pas.rochester.edu/~martinhe/2011/agn-6apr-dens1.gif

See updated in:

Binary ​https://clover.pas.rochester.edu/trac/astrobear/blog/binaryBondi

AGN jet truncation ​https://clover.pas.rochester.edu/trac/astrobear/blog/agnJetTruncation

PN wind paper. Waiting for reply from Raghvendra, Adam and Bruce t resubmit to MNRAS.

I plan to show images on some of the projects during the meeting.

Binary.

-Embedded disks in an AGB wind. The 1st test has been running in bgene since Sunday morning. I do not see a strong tilt so far, but gas in the innermost orbits does show some tilt.

No. density iso-surfaces for the case with a disk tilted 30o, facing the primary. rdisk=rBondi/3 to make the test run faster.

-40au tests, see the table of 29th March at ​https://clover.pas.rochester.edu/trac/astrobear/blog/binaryBondi. Only run 7 is still running. The others were killed during a weekend bgene maintenance session. I've requested another reservation to continue working on these runs.

-Velocity field 2-plane evolution. I'll soon start doing the movie we discussed last friday.

CRL618

-See ​https://clover.pas.rochester.edu/trac/astrobear/blog/crl618Figures for new movies.

-Bin will present a poster about this in about a week time.

AGN jet truncation. See ​https://clover.pas.rochester.edu/trac/astrobear/blog/agnJetTruncation for new movie.

Magnetic tower paper submitted!, ApJ page charges? HEDLA talk?'

Teragrid. Baowei and I are doing the final few installation steps needed to run the code at ranger.

I'll post images soon.

I'll submit the magnetic tower paper to ApJ and arxiv this Friday.

Binary

• The 40AU run with the parameters discussed last Friday is running. It's now at its early phase and seems to be doing well.

I'm working on plots of mean angular momentum vs time. I've used the data from the simulation that showed a tilt of 90deg (see last week's post). I've only had time for a quick inspection. The facts that jz is negative (because particles orbit clockwise) and larger (about 300 times) than the other ang. mom. components, are expected. Trying to understand the gradients in plots and the relative values of the momenta.

AGN jet truncation by stellar winds. The 1st test of Model 2 is still running. It's a little more than half way though. The RG's wind looks square-ish because of (i) the decreasing radial resolution of this test (see ​https://clover.pas.rochester.edu/trac/astrobear/blog/agnJetTruncation. This will be fixed for production runs) (ii) the very high density contrast with the ambient medium. The stellar wind's momentum in this case is rather strong and able to truncate the very light AGN jet, despite the fact that the latter is about 700 times faster. I plan to start running Model 3, milder stellar wind, by weeks end or early next week.

PN wind. I'm working on the referee's suggestions. Have not finished yet. See progress in Figures 2, e.g. , 3, 4 and 5, as well as the new section 4.2 in ​http://www.pas.rochester.edu/~martinhe/PNpaper-mnras2.pdf. Plan to send it to Adam, Eric and Raghvendra soon.

CRL618. The jet version of the runs with a toroidal AGB and higher densities, with and without ambient rings, are running. Should finish by week end.

Quick look

Binary

See ​https://clover.pas.rochester.edu/trac/astrobear/blog/binaryBondi for images and movies.

• In general, for times <~ 1orbit, the 40 AU runs form strongly tilted disks with angular momenta vectors which are
  • contained very close to the orbital plane
  • point at the winds incoming direction; ~10^o from the primary's position.
• This tilt seem independent of:
  • the soft radius
  • whether the gas initial condition is a light static ambient medium or the AGB wind
  • q, for I tried for q=m₁/m₂=1.5,2
  • the secondary's spin
• The formation of this structure is ~4 times faster for r_soft=0 than for r_soft=2dx
• I see a less pronounced tilt in a 11au run (see ​https://clover.pas.rochester.edu/trac/astrobear/blog/binaryBondi 20 mar '12)
• The tilt doesn't happen in runs with:
  • a<~5au separation (as in M&M)
  • more resolution (because the 11-40au grids are larger) to see the Hill radii. I've not used more resolution yet, for these sims running times are rather large and wanted to see if I could get disks in sensible walltimes.
  • the 2 conditions above + v_wind=20km/s
• I do not fully understand why such a dramatic tilt in the 40au case, yet the wind velocity, the shear and the wind density near the secondary's position, are all higher in the 11au sims than in the 40au ones. Also, the No. of cells per r_Hill scales down with the size of the grid.
• As reported by email, one of my 40au test produced a disk on the orbital plane, but for:
  • an initial AGB wind with a density perturbation (which are expected in AGB stars; i.e. early pulsations)
  • boundary inflow, which was not intended.

I found the tilt again once I removed both the boundary inflow and the wind density perturbation. I'd like to try the perturbation again (without the inflow).

Next steps:

• 40 au runs with higher resolutions
• Longer runs
• these runs should take about 1.5-2 weeks to run, even with the sandwich grids I'm using which, BTW, are enough to resolve Hill radii. I've not seen significantly faster runs in bluegene so far. I suspect, however, based on previous tests, that the bluegene sims will stop due to the error reported in ticket 121.

CRL618, several new plots and movies at ​https://clover.pas.rochester.edu/trac/astrobear/blog/crl618Figures#comment-1

AGN jet truncation. Model 2 is running now, see ​https://clover.pas.rochester.edu/trac/astrobear/blog/agnJetTruncation

Magnetic tower. Waiting for comments from Eric, Pat, Sergey and Jerry. Will submit to ApJ next friday.

PN winds. I'm working on the referee's suggestions, see Figures 2,3 and 4 in ​http://www.pas.rochester.edu/~martinhe/PNpaper-mnras2.pdf

Color figures for the printed version?

Binary.

I'm continuing working on the 40AU case. High res sims have produced a "disk-like" structure, the angular momentum vector of which seems to point towards the primary. It doesn't make sense to me. I'm investigating this but suspect it may be related to the fact that the secondary pulls before the it is inside the wind (I used this setup for it worked well for our previous runs with Bondi accretion and smaller separations). I want to restart the sim (i) once the secondary is inside the wind (ii) with a secondary which starts pulling gas after restart. The restart procedure has changed in the latest code revisions, so I'm updating my module. IMAGE: 2d density maps showing a part of the orbital plane close to the secondary. Left: rsoft=0; Right: rsoft=dx. Times are different in each panel.

CRL618.

The tracer field that represents the DM cooling seems to be working well. This sim ran 40% and is scheduled to restart in bgenen soon.

As discussed last time, I increased the densities of both the clump and the ambient medium by a factor of 10 in order to get stronger cooling and thus thinner lobes. In addition, the AGB wind is toroidal. Here's and image from the low res test, the high res one should run soon.

PN paper. I've heard back from MNRAS: "…Minor revision of your manuscript is requested before it is reconsidered for publication."

Magnetic tower. Waiting for comments from Adam, Eric and Pat to submit. I had a discussion with Manoj and he's very interested in out magnetic towers to model some of their recent Hershel observations. He scheduled a talk for me and will ask Adam to give one, in a meeting that he, Dan and other people will have in Rochester in about 3 weeks.

AGN jet truncation. As I said last time, the RG wind looks strange for it is subsonic. New runs:

1. smaller grid and jet radius by a factor of 2 + more refinement levels,
2. same as 1 but for a jet kinetic luminosity of 10⁴⁵ers/s (instead of 4x10⁴²),
3. same as 1 and 2 but for a magnetized jet. Should have an effect on the RG wind.

-Binary. I've ran 3 tests with a=40au. I have not seen the formation of a disk after 1 orbit. I suspect this happens because I'm using a ~4-times smaller resolution than before, because of the larger value of a. Here's an image of the run:

Left: Zoom in to see the secondary, showing the log density (cu) and the velocity field in Mach units. Material is pulled towards the particle but does not go about it. Right: vel field on the entire orbital plane. AGB is in the upper left while the secondary is on the bottom right. The latter does't seem to affect the wind strongly. Either the wind is too fast, 15km/s, too dilute, M'=1x10-5Msun/yr, or the gravitational pull of the secondary (1Msun, rsoft=2cells, 1283 + 4 particle refs.) is weak.

I'm now running a higher res version of it.

-Magnetic tower:.

• Andrea has replied, he's happy with the paper.
• I've calculated the volume time average mean flux ratios, <Q> in the following way. However, Eric and I agree that this volume calculation is not well defined for the fluxes; they should be taken on horizontal slices through the jet beam, thus we believe that Figure 7 in the paper (logarithmic flux rations color maps) does convey the fact that our towers remain, as they should, PDF from base to head, throughout the sims.

The volume calculations:

(1/N_cells) SUM_x,y,z [ f_P(x,y,z,t)/f_k(x,y,z,t) ], (1)

where x,y,z are cells inside boxes which contain:

• (i) the jet (RIGHT PANEL; x,y ⇐ |r_jet|; z⇐ height_cavity)
• (ii) the whole magnetic cavity (LEFT PANEL; x,y ⇐width_cavity; z⇐ height_cavity).

The time averages of the above:

SUM_t { (1/N_cells) SUM_x,y,z [ f_P(x,y,z,t)/f_k(x,y,z,t) ] }, (2)

where t = 42,84,118. These yield, <Q>_jet~ 21; <Q>_cavity~14.

-CRL618:.

• I've implanted a tracer field which takes the values of the energy loss due to cooling. Will give us a better idea on the emission of our nebulea.
• I've been doing low-res tests with a toroidal AGB (ambient medium) distribution using eq (13) from our PN paper, but with other, more torus-like, alpha and beta values. I've added the ambient shells to this as well. I see (i) concave, rather than a round, bow shocks, (ii) lobes with very similar, or smaller (fatter), aspect ratios than the ones produced with a spherical ambient. Not sure this is helping to get CRL618-looking objects.

-AGN jet truncation. Eric and I have discussed the relative speeds, densities and temperatures of the ambient, red giant (RG) stellar wind and the AGN jet. Here's our latest test run:

​https://clover.pas.rochester.edu/trac/astrobear/blog/agnJetTruncation

We study the 3D interaction of stellar winds from red giant (RG) stars and AGN jets. We're based on

¹​http://adsabs.harvard.edu/abs/2006MNRAS.371.1717H

Note this blog is in chronological order.

6 june '12

Latest sim ​http://www.pas.rochester.edu/~martinhe/2011/agn/hd-strongJet-edge2.gif shows that the red giant's (RG) wind, which crosses the edge of the jet's beam, strongly affects the collimation of the AGN jet. Note that in the previous sim ( ​http://www.pas.rochester.edu/~martinhe/2011/agn-6apr-dens2.gif) the RG's orbital path intersected the jet's axis, affecting the jet's beam more drastically.

9 Apr '12

The other parameters are as in Run 3 (below) except for:

• the jet is launched earlier
• the RG's initial position is farther form the jet's axis

No. density movie: ​http://www.pas.rochester.edu/~martinhe/2011/agn-6apr-dens2.gif

I see that a reconfinement shock forms in the jet, the height of which increases in time and, at this point, is at a height close to the RG path. These shocks are expected⁺ and seen in many other agn jet sims. This process enhances the jet's kinetic energy flux at that height, hence affecting the winds' interaction.

⁺​http://adsabs.harvard.edu/abs/1991MNRAS.250..581F

2 Apr '12

Because of the opening angle of 5^o , the jet has a density contrast of 0.0001 with respect to the ambient medium at the position of the RG, 1100pc from the origin

No. density movie: ​http://www.pas.rochester.edu/~martinhe/2011/agn-dens-2apr.gif

14 March '12

^* Because of the opening angle of 5^o , the jet has a density contrast of 0.001 with respect to the ambient medium at the position of the RG.

The jet will be launched once the star has reached the middle of the grid in the horizontal direction, not the other way around.

13 March '12

Meeting with Eric and Martín. We found, by taking the momentum ratio of the jet over the star on the interception surface, that the back force of the jet upon the star is very weak; several orders of magnitude. The passage of the star though the jet beam is ~ 10⁵ yr.

New runs:

• Run 2: as Run 1 (below) but (i) 8 times more resolution by a combination of grid size, jet radius and refinement level. (ii) The jet will be launched once the star has reached the middle of the grid, not the other way around.
• Run 3: as Run 2 but with L_jet-kinetic=10⁴⁵ erg/s and the corresponding jet density for vel_jet=.5c,
• Run 2.1: as Run 2 but with a magnetized jet with beta=1, the geometry of which will be decided later.
• Run 3.1: as Run 3 but with the magnetized jet of Run 2.1.

3 March '12

^* Because of the opening angle of 5^o , the jet has a density contrast of 0.001 with respect to the ambient medium at the position of the RG.

The sRG enters the edge of the grid with a horizontal velocity of 200km/s once the jet's head has reached a third of the grid along the vertical direction.

Run time=2.3days, 24procs, afrank, bluehive

Log No. density movie. The jet's bow shock quickly leaves the grid and affects the RG's wind spherical structure (bright small structure on the left). The simulation takes place inside the cocoon then. The jet is not truncated; it's quite strong relative to the wind, in agreement with¹. The interaction of the wind and the jet's beam edge affects the structure of the cocoon asymmetrically. A boundary effect rises affecting the jet beam structure near the base. It relates to the grid structure, easy to solve.

​http://www.pas.rochester.edu/~martinhe/2011/agn6mar.gif

Mach No. The shape of the RG wind is amorphous, not spherical, despite that fact that I do inject a spherical wind, for it is subsonic in relation to the cocoon material.

​http://www.pas.rochester.edu/~martinhe/2011/agn8mar.gif

• Binary: ​https://clover.pas.rochester.edu/trac/astrobear/blog/binaryBondi

• CRL618: We need to met and discuss what Adam and Bruce chatted about last week.

Preliminary look at a 2 clumps, one after the other, run made with periodic BC. The initial dens-contrast was 100 (twice as in the previous models, in order to have sensibly dense 2nd clump). The simulations in which I placed the 2nd clump into the grid, once the 1st one had left, generated cfl and nan errors which led to infinitesimally small dt. A wider grid needed. Yet, the lobe structure generated by the ambient shells-1st clump interaction is erased by the 2nd clump. Also, 2nd clump generated shocks should have quite low temperatures, may be hard or imposible to observe. ?

MOVIE

Now working on the run to produce a cooling map.

• Magnetic tower paper. Sent though for final revision. Some plots about the flux ratio, which I have not included in the paper:

• PN paper submitted to MNRAS

• AGN jet truncation. Managed to make the code cope with real high Mach numbers, order 100, for these runs. These are needed because of the large differences of temperature and velocity between the AGB wind and and the AGN jet. Meeting with Eric this Friday, 2:30pm, to discuss this. Test runs looking good.

Check out the following pages for updates.

Binary. ​https://clover.pas.rochester.edu/trac/astrobear/blog/binaryBondi The central diks test + Bondi accretion

CRL618. ​https://clover.pas.rochester.edu/trac/astrobear/blog/crl618Figures (I've added movies and updated 2d color scale density maps for the ones with higher resolution). The run with 2 sequential clumps in bluegene's queue.

PNe paper for MNRAS. Orsola is reading it. I will submit tomorrow.

Magnetic tower paper. Adam is reading it.

I've sent the teragrid proposal.

I've resumed work on the AGN jet truncation project.

Dennis et al.: ​http://adsabs.harvard.edu/abs/2008ApJ...679.1327D

New site with info for the paper: ​https://clover.pas.rochester.edu/trac/astrobear/blog/crl2013

17 dec

Short AGB rings separation, v_bullet=300km/s model, inclination angle of 30^o

TESTS Integrated "Doppler-shift" image. This is the bullet model at 200yr, 30o inclination angle, and only velocities from 10-50 km/s are mapped (based on a phone discussion with Bruce; I could map any other vel components if wanted).
Ditto with the "red-blue" Shape table.

Time [yr]	50	100	200
non-integrated density maps [part cm-3] and velocity field comparison Logarithmic false gray-scale density maps and color velocity field on the plane at the middle of the computational domain. Left panels show the bullet model, while right panels show the jet model. The bullet/jet are the densest, whitest, central features. Behind the bullet, or to the right of the jet (without loss of generality), we see the cavity formed by the bullet/jet, which is separated from the ambient medium by a contact discontinuity. The ambient medium is stratified and shows a series of concentric spherical shells (see Section "Initial conditions"). The vertical short red, or blue, lines at the top of the maps show the positions at which the lineouts of Figures X Y have been taken. The bullet and the jet propagate at 300km/s away from the ambient medium's densest region (up), forming an elongated lobe. Comparing the left and the right panels in FIGURE X [gray-scale density maps], we find that the lobes formed by the bullet and the jet are quite similar. As the bullet (jet) penetrates the ambient's shells, these form regularly separated vertebrae-looking features along the lobe. The axial velocity of these features decreases with radial distance from the axis.
non-integrated density lineouts [part cm-3] comparison. See top row for lineouts' positions.
non-integrated vel. lineouts comparison. See top row for lineouts' positions.
Cooling emission, slit marked in blue, Bullet
Cooling emission, slit marked in blue, Jet
PV diagrams, Bullet
PV diagrams, Jet

5 Dec 2012, long AGB rings separation, v_bullet=200km/s model

Time [yr]	50	100	200
non-integrated density maps [part cm-3] comparison
integrated Emission & non-integrated vel. comparison
non-integrated density lineouts [part cm-3] comparison. See top row for lineouts' positions.
non-integrated vel. lineouts comparison. See top row for lineouts' positions.

2 Apr '12

• Clump/Jet to ambient density contrast of 100 (was 50)
• Toroidal AGB wind, based in Frank & Mellema '94, alpha=.7 and beta=.8
• Higher initial densities
• 128x128x192+2AMR levels (~4 days to run in 1024 bgene procs)

There are some spurious numerical artifacts ahed of the jets' head at late times.

16 mar '12

14 feb '12

Clump/jet velocity of 400 km s^-1, dens_clump/dens_amb=50, larger grid.

Lineouts are taken along the lines marked in this figure >

Clump, stratified and ringed ambient medium:	t=88yr	t=176yr	t=247yr
Log(dens) maps. MOVIE: ​http://www.pas.rochester.edu/~martinhe/2011/crl/clump-ring-dens.gif
Log(dens) axial lineouts
Axial vel lineouts
Clump, stratified ambient medium:	t=88yr	t=176yr	t=247yr
Log(dens) maps. MOVIE: ​http://www.pas.rochester.edu/~martinhe/2011/crl/clump-dens.gif
Log(dens) axial lineouts
Axial vel lineouts
Jet, stratified and ringed ambient medium:	t=88yr	t=176yr	t=247yr
Log(dens) maps. MOVIE: ​http://www.pas.rochester.edu/~martinhe/2011/crl/jet-ring-dens.gif
Log(dens) axial lineouts
Axial vel lineouts
Jet, stratified ambient medium:	t=88yr	coming soon	ditto
Log(dens) maps. MOVIE: ​http://www.pas.rochester.edu/~martinhe/2011/crl/jet-dens.gif
Log(dens) axial lineouts
Axial vel lineouts

SYNTHETIC IMAGES

Ambient =r^-2 + rings, time~176yr, the slit is r_jet/2 displaced from the symmetry axis

Inclination	Clump, log(rho2)	Clump, pv		Jet, log(rho2)	Jet, pv
90o
60o

Ambient =r^-2, time~176yr for the clump and time~88yr for the jet (still running), the slit is r_jet/2 displaced from the symmetry axis

Inclination	Clump, log(rho2)	Clump, pv		Jet, log(rho2)	Jet, pv
90o
60o

Bruce's thoughts

RED IS SHOCK-EXCITED [NII] GREEN IS HALPHA — MOSTLY COMING FROM THE STAR BLUE IS MOSTLY SCATTERED STARLIGHT ============== CO observations regarding the ambient medium

take a look at Fog 2 and the rest of Sa ́nchez Contreras, C., Sahai, R., & Gil de Paz, A. 2002, ApJ, 578, 269 (optical emission-line study of CRL618): ​http://iopscience.iop.org/0004-637X/578/1/269/pdf/55888.web.pdf)

Here's my summary of the highlights of this paper

Fig 2 shows long-slit P-V diagrams of selected emission lines. Scattered stellar Halpha is significant near the center, and the Halpha line is thermally broadened everywhere. The other lines show a linear rise in V with slit position from the star…close to a Hubble flow. But the lines don't arise from the insides of the fingers. They come from an outer sheath where the lateral expansion of the fingers produce shocks. (Inclination corrections are important in the interpretation of these spectra.) (Note: one might expect two velocity components at each position arising from the near and far sides of the laterally expanding fingers. This isn't seen, but the limited dispersion of the spectrograph could be the reason why. Our models need only explain the general trends of the P-V diagrams.

The optical fingers are relatively low- and constant-density outflows (~5000 cm-3) plowing through a denser and slower AGB wind (10^{6 cm-3; 18 km/s). The density of the AGB wind appears to decline as r}-2. The shock temperatures (shock speed) derived from emission lines range from 10,000 to 25,000K (75-200 km/s). (They do not directly measure the temperatures along the fingers and through the tips using emission line diagnostics such as [NII]5755/6584.)

The optical emission in the fingers consist of (1) scattered starlight, (2) scattered Halpha and other emission lines (e.g. [OIII]) from a small, dense (10^{6 cm-3, T~14000K) HII region within 0."4 of the core, and (3) shocked gas at the interfaces along the edges and at the tips of the fingers. (Scattered light from the HII region is seen inside the lobes but at different velocities than the intrinsic emission from the lobes.)}

The shock speeds needed to explain the observed emission-line ratios are 75-200 km/s. An independent measure of v_shock at the fingers tips comes from the width of emission lines at the tips of the fingers: 200-230 km/s. The shocks can cross the fingers laterally in a few years.

The inclination angle of the fingers is 24 ± 6 deg, so the predicted space motions of the tips are 80/tan24 = 180 km/s, in good agreement with the estimated shock speeds

The shocks along the edges of the fingers are radiative (detailed discussion in section 9 p 286). The cooling time behind the shock is weeks. So energy from an ongoing fast wind is needed in order to maintain the radiation in the finger edges

The measured density along the length of the fingers is 5000 cm-3 with only small and local variations. This constant density contrasts with the density distribution of the surrounding neutral gas.

(BB: question for the Rochester crew: according to models, will the jets accelerate as they plow through decreasing ambient density? About knots, how will the general shapes of the fingers differ in an external medium that is (1) uniform, (2) declining as r^{-2? Can we use the shapes of the fingers to deduce the density falloff in the external medium?)}

============== More recent CO observations with somewhat higher spatial resolution and a spatio-kinematic model of the ambient molecular cloud

============== (movie 1)

============== Martin, two of the most notable features of the evolving structure of CRL618 are the motions and brightness changes of the tips of the fingers. This is seen on the 3-frame movie that's attached. open it with a browser. The movie frames are from 1998, 2002, and 2009 (not equally spaced)

One thing that we have yet to explore with the models is the changes in tip brightness as the tips cross the rings in the dust distribution. One might expect them to brighten as the bullets or jets encounter rings of higher density and to fade in between. In fact, after I stare at the movie, I think that I see the reverse…the tips fade when they hit the rings. Of course, the enhanced foreground extinction will affect the optical brightness.

Too bad that we don't have an IR move of the fingertips!

movie 2

============== Balick's first thoughts on the models 92/10/12)

FILES:

• ​http://www.pas.rochester.edu/~martinhe/2011/crl/PastedGraphic-1.tiff
• ​http://www.pas.rochester.edu/~martinhe/2011/crl/CRL618residmovie.gif
• ​http://www.pas.rochester.edu/~martinhe/2011/crl/crl618.f656-606-656movie00.gif
• ​http://www.pas.rochester.edu/~martinhe/2011/crl/CRL618.f547m.2009.6-1998..pdf
• ​http://www.pas.rochester.edu/~martinhe/2011/crl/Hydro_comments.pdf

Older model info

• ​https://clover.pas.rochester.edu/trac/astrobear/blog/author/blin
• ​https://clover.pas.rochester.edu/trac/astrobear/blog/syntheticImages
• ​https://clover.pas.rochester.edu/trac/astrobear/blog/martinhe01202012

Embedded disks in the AGB wind. I've ran two sims:

1. a disk contained in the orbital plane,
   • log density movie (upper part of the orbital plane, initially the disk is on the left and the AGB on the right): ​http://www.pas.rochester.edu/~martinhe/2011/binary/binary-n-disk1-dens.gif
   • vx movie (same display setup as the dens movie above): ​http://www.pas.rochester.edu/~martinhe/2011/binary/binary-n-disk1-vx.gif

I've only glanced at these movies and data, so the following are simple observations which need some serious thought.

• The structure of the disk is quickly lost
• The disk's former gas evolves and adoptes a structure which looks like the tilted disks of the binary sims (see table below).
• There is a shock wave coming from the AGB. This happened because I didn't adjust the density to match the one corresponding to the low resolution I used for this test. Yet, seems the diks looses its structure before the shock reaches the secondary's radius. I'll fix this for future tests, if any.

2. a disk with an ang. mom. vector at an angle of 30^o with the orbital ang. mom. vector.
   • log density movie (upper part of the orbital plane, initially the disk is on the left and the AGB on the right): ​http://www.pas.rochester.edu/~martinhe/2011/binary/binary-n-disk2-dens.gif
   • vx movie (same display setup as the dens movie above): ​http://www.pas.rochester.edu/~martinhe/2011/binary/binary-n-disk2-vx.gif

29 Mar '12

a=40 AU tests.

About run speed. It is proportional to:

1. the resolution

1.1 dx_max / dx_min

2. the filling ratios. They are not crucial for these sims because I'm using particle refinements, not to the AMR (which will not really help to seed up the runs). Yet, I control the radii of cells of each level, taken form the particles' center. I've adjusted these to be small enough to aid the run speed but large enough to capture the AGB wind and the Bondi radius.
3. dt, which is proportional to cfl*dx_min/ max(v_w, c_s, v_orbit)
4. the No. of processors used, N_p
5. cluster communication and processors' clock speed
6. the advance speed (computation time per grid level).

My tests indicate that for separations ≥ 20AU, the resolution should be >~ .047AU (64³+5refs) to form disks. I consistently see that bhive's runs are faster than bgene's (even when I use four times more processor in the latter than in the former). What worries me is the advance speed. The code's output shows that the simulation spends a good deal of time in this process. e.g. test 6 (column 6 in the table below) shows advances between the levels 4, 5 and 6 (which go back and forth several times between each level 0 dt) take as long as 12 secs. So every full timestep advance takes ~minuts to happen. Why, and how can I improve this?

r_B=2Gm₂/(v_w² + c_s² + v₂²) [from ^*],

r_B^'=Gm₂/(v_w² + c_s²) ,

where r_B, m₂, v_w, c_s, and v₂ are the Bondi radius, the secondary's mass, the sound speed and the secondary's orbital velocity with respect to the center of mass.

Test	q=m1/m2	resolution	rsoft/dx	rB/dx	rB/rsoft	rB'/dx	rB'/rsoft	Tw [K]	vw [km/s]	M'w [10-5Mo/yr]	time [orb]	log(dens/cu),vel/Mach
1 (bgene, "Rsoft8")	1.2/.6=2*	642x16+6refLev, dx=.023AU	2	448.7	224.3	272.1	136	300*	15	1	.016
2 (bgene, "2", running)	1.2/.6=2*	1282x32+6refLev, dx=.011AU	2	448.7	224.3	544	272.1	300*	15	1	.002
3 (bhive)	1.2/.6=2*	642x16+7refLev (slightly larger grid), dx=.015AU	6	718	119.6	435.3	72.6	300*	15	1	.102
4 (bhive, "2", running)	1.2/.6=2*	1282x32+5refLev, dx=.023AU	3	448.7	149.6	272.1	90.7	300*	15	1	.061
5 (bgene, "3", running)	1.5/1=1.5+	1282x32+5refLev, dx=.023AU	2	693	346.6	424.1	212.1	1000	15	10	.008
6 (bgene, "4", running)	1.5/1=1.5+	1282x32+6refLev, dx=.011AU	2	1386.4	693.1	848.2	424.1	1000	15	10	.001	< tilt
AGAIN 6 (bgene, "4", running)											.0027a
7 (bhive, "3", running)	1.5/1=1.5+	642x16+5refLev, dx=.047AU	4	301.1	75.3	179	44.7	3000	9	2	.062

^* val-Borro et al.

⁺ M&M '98

^a ​http://www.pas.rochester.edu/~martinhe/2011/binary/gene-4.gif

20 mar '12

As in M&M '98, model 1. I did a similar test before (see 21 feb '12 post), but it was shorter, with less resolution and with a separation

• Temp=3000K
• AGB mass-loss = 10^-5 M_o yr^-1, from time=0
• vel_wind=9 km/s, from time=0
• a=40AU
• circular orbit
• q=1.5 (m₁=1.5; m₂=1 M_sun)
• r_soft=2
• 64x64x16cells + 5 particle grid refinements
• grid: x,y ⇐|32AU|; z⇐|8AU|.

Running the same model but with r_soft=0.

As in Val-Borro et al. '09 (​http://adsabs.harvard.edu/abs/2009ApJ...700.1148D)

• Temp=1000K
• AGB mass-loss = 10^-5 M_o yr^-1, from time=0
• vel_wind=10 km/s, from time=0
• a=40AU
• circular orbit
• q=2 (m₁=1.2; m₂=.6 M_sun)
• r_soft=2
• 64x64x16cells + 5 particle grid refinements
• grid: x,y ⇐|60AU|; z⇐|15AU|.
• Running time (24 afrank p, bluehive) = 4 days

Log(dens) on orbital plane

Here are some snapshots of the orbital plane velocity field, ​http://www.pas.rochester.edu/~martinhe/2011/binary/40au-bb5-vel.pdf

Here are some plots of the mean angular momentum in the grid as a function of time, ​http://www.pas.rochester.edu/~martinhe/2011/binary/mAngMom.png

28 feb '12

As in M&M '98 model 3:

• Temp=2400K
• AGB mass-loss = 10^-5 M_o yr^-1 (they actually use 8x10^-6)
• a=17AU
• vel_wind=15 km/s
• circular orbit
• q=1.5
• r_soft=2
• 128x128x64cells + 4 particle grid refinements
• grid: x,y ⇐|25AU|; z⇐|12.5AU|; runs faster. I've checked and there's no boundary inflow.

Density iso-contours, edge-on, time=.5 orbits, zoom in. No tilting. The captured wind does show a disk-like shape, but at this point the disk is forming.

24 feb '12

Same model as yesterday, time=2 orbits. There's some inflow from all the boundaries onto the grid (left panel, small v_z from all boundaries), so I need a larger, or a cubic, grid and/or wind objects to block the inflows. Easy to solve. The inflow makes the flow patten quite messy and destroys the spiral structure induced by the orbit (middle panel, orbital plane view). The disk is not strongly affected by the inflow, which is good (right panel, low-res perspective view of iso-contours showing that the disk is plane symmetric and has an asymmetric bow shock which faces the AGB star).

I'll stop this simulation and send another one with the same setup but: a cubic grid and outflow-only wind objects at the boundaries.

23 feb '12

A very handsome disk!!'''

• Temp=3000K (as in M&M '98)
• AGB mass-loss = 9.9x10^-6 (as in M&M '98)
• a=3.7AU < M&M '98
• vel_wind=9 km/s (as in M&M '98)
• circular orbit
• q=1.5 (as in M&M '98)
• r_soft=2
• 128x128x64cells + 4 particle grid refinements⁺
• grid: x,y ⇐|1|; z⇐|.5|. Runs faster. We can use the full cubic grid for production runs.

Next steps:

1. try M&M '98 model 4.
2. elliptical orbit

⁺ Runs faster (1 orbit per 16 running hrs) than 32x32x16+6 particle refs (based on another test using 32³ cells +5 particle refinements which produced 1 orbit per 17 running hrs; yet for the latter test I used r_soft=0 which produces high velocities in the central-most orbits of the disk, hence reducing the timstep); the more grid refinements I request, the grater the numer of sub-steps the code has to perform. This is for 48 afrank processors.

22feb '12

Time=2.7orbits, no tilt.. The secondary keeps accreting mass and capturing wind material. I still see significant density gradients in the bound gas. Mastrodemos & M do not see this, so I think this is purely a shock effect. De Val-Borro et al. do see something similar, specially for their large wind region models (​http://adsabs.harvard.edu/abs/2009ApJ...700.1148D), but this may be a 3D effect. This image shows 5 flow steam lines of the wind captured gas.

I want to run this problem again with 1 more refinement level and a r_soft=2dx which should reduce the velocity of the central most cells. I presume this will make the disk radius larger.

21 feb '12

As in M&M '98 model 1:

• Temp=3000K
• AGB mass-loss = 9.9x10^-6
• a=3.7AU
• vel_wind=9 km/s
• circular orbit
• q=1.5
• 32³ + 5 particle grid refinements
• r_soft=0

I see a disk-looking structure (with a larger radius than the one in the previous test), with a Keplerian-like vel distribution and a flow structure that's symmetric with respect to the orbital plane (i.e. no tilting), after~1.3 orbits. The simulation is still running. I want to see it at 5 orbits.

Log density in grayscale. Velocity field in color scale in Mach units.
Zoom in to the disk

Central disk + Bondi:

I do not see tilting in the central region of the disk. Note that for this setup (taken from test 2*) rsoft=4dx, hence the particularly soft-looking center of the disk. This is about 25% of the run time that I used in test 2*, but it is well within the tilting growing time.

^* ​https://clover.pas.rochester.edu/trac/astrobear/blog/martinhe02032012

20 feb '12

As in M&M '98:

• Temp=2400K
• AGB mass-loss = 9.5x10^-6
• a=12AU (they actually have 12.6 AU)
• vel_wind=25km/s
• circular orbit
• q=1.5
• 32³ + 4 particle grid refinements
• r_soft=0

I see a disk-looking structure, although smaller than I expected, after~7.5 orbits. Again, it is symmetric with respect to the orbital plane, hence Jonathan's Bondi accretion implementation see to have solved the tilting enigma. I need more resolution to capture the full formation of the disk.

15 feb '12

Same as below but 64³ + 5 particle grid refinements and temp_wind=1000K (and in an exploratory elliptical orbit)

PRELIMINARY: I see a disk-looking structure after~3.7 orbits which is symmetric with respect to the orbital plane!!

14 feb '12 Jonathan has implemented, and tested with a central disk problem setup, the Bondi accretion of sink particles. I've been trying it in one instance of my binary-formed disks problem with:

• isothermal solver, gamma= 1.001
• r_soft=0 (as suggested by Jonathan)
• a=20 AU
• q=1.5
• vel_wind=20km/s; temp_wind=2000K (line M&M '97); mass-loss_wind=10^-5 M_sun /yr
• 64³ + 3 particle grid refinements, so dx~2.1 AU
• r_Bondi=4 AU; r_Bondi/r_soft=NA

I do not see a disk even after 20 orbits. The wind captured structure does look different than the one formed without* the Bondi accretion. I.e. it shows a light core and a dense tail (see left and upper right panels), but not the other way around (as in * ). Also, the structure is symmetric with respect to the orbital plane (see lower right panel).

I'm now trying this setup, but with these changes:

• 5 particle grid refinements ( not 6 yet for it will be rather slow), so that r_Bondi=8dx (instead of 2dx)
• temp_wind=1000K, instead of 2000.

^* see test 1 in ​https://clover.pas.rochester.edu/trac/astrobear/blog/martinhe01292012

CRL618

14 feb '12

Clump: 400 km s^-1, dens_clump/dens_amb=50, larger grid

Ambient =r^-2 + rings, time~176yr, the slit is r_jet/2 displaced from the symmetry axis

Inclination	Clump, log(rho2)	Clump, pv		Jet, log(rho2)	Jet, pv
90o
60o

Ambient =r^-2, time~176yr for the clump and time~88yr for the jet (still running), the slit is r_jet/2 displaced from the symmetry axis

Inclination	Clump, log(rho2)	Clump, pv		Jet, log(rho2)	Jet, pv
90o
60o

9 feb '12

Clump: 400 km s^-1, dens_clump/dens_amb=50

Model C^*: ambient =r^-2 + rings, time~120yr

Clump	log(rho2)	pv
90o
60o

Model C^*: ambient =r^-2 + rings, time~120yr

Clump+ambient	log(rho2)	pv
90o
60o

^*​https://clover.pas.rochester.edu/trac/astrobear/blog/martinhe01202012

• ideal gas solver, gamma=1.1
• temp_disk=1K; temp_amb=1000K
• dens contrast=10³
• r_soft=4= .5 disk_height
• r_disk=2 cu (=20AU)
• 64³ +2amr
• periodic BC

The gas evolution in this simulation is as expected and consistent with my previous tests (see tables 1 and 2 in ​https://clover.pas.rochester.edu/trac/astrobear/blog/martinhe12092011).

Check out updates in ​https://clover.pas.rochester.edu/trac/astrobear/blog/martinhe01202012

• Cold, temp=10K
• r_soft=0
• flared
• dens contrast=10³ (less than in tests 2, 2.1 and 3^*),
• High time resolution
• 64³ +2amr
• the disk has not been rotated
• r_disk=2 cu (=20AU; r_disk=1cu in test 2 and 2.1^*)
• periodic BC (note that the domain goes from -6 to 6cu (1cu=10AU), so the disk is till far from the boundary)

The central tilt happen again and quite quickly. There's no disk gas located at r < r_soft in this case. The knee shown by the dens distribution, i.e. the tilt, is also followed by the velocity distributions.

^*​https://clover.pas.rochester.edu/trac/astrobear/blog/martinhe01292012

This is the same as test 3 (​https://clover.pas.rochester.edu/trac/astrobear/blog/martinhe02032012) but the disk is initially inclined by 10^o with respect to the xy plane.

Central disk tilt is still evident, so seems that the grid coordinates, and split solving, are not introducing numerical artifacts which may cause the tilt.

I've been trying to run the binary wind capture simulation using the reservation that we have in bluegene. I have however found the bug in ticket 121 (​https://clover.pas.rochester.edu/trac/astrobear/ticket/121). i.e., the code runs for a short while, aborts and reports:

hyperbolic/sweep/i_dependencies.f90", line 548: 1525-108 Error encountered while attempting to allocate a data object. The program will stop.

I do not see the error in bluehive (~ 32 afrank procs). I cannot go any further in bluegene with the following parameters:

• built at gbene, /home/mhuartee/27nov/
• revision 696
• ran at /scratch/mhuartee/astrobear2/feb-reserva/c, where all the relevant files (Makefile.inc, submit.cmd, *.data, binary ad chombo) are located and have open permissions
• job ID 36691
• 256procs
• produced one 25MB chombo00000 only (because I had set it to do so)
• the amr was off via: desieredFillRations=0 0 …; qTolerances=1e30 1e30…; refinemetVariableFactors=0 0 …
• 5 levels of sink particle refinement.

$> cat core.0 | addr2line -e ./astrobear

shows:

…

source/pointgravity.f90:352

source/pointgravity.f90:349

hyperbolic/sweep/sweep_scheme.cpp.f90:3571

hyperbolic/sweep/sweep_scheme.cpp.f90:3571

modules/objects/disks.f90:290

modules/objects/disks.f90:312

modules/objects/disks.f90:82

modules/objects/disks.f90:73

modules/objects/ambients.f90:128

modules/objects/outflows.f90:593

modules/objects/outflows.f90:279

modules/objects/outflows.f90:510

particle/particle_declarations.f90:568

modules/objects/outflows.f90:289

data/data_info_ops.f90:2513

data/data_info_ops.f90:2418

data/data_info_ops.f90:1961

data/data_info_ops.f90:1961

data/data_info_ops.f90:2024

data/data_info_ops.f90:2106

data/data_info_ops.f90:2091

…

I do not trust this error message since I've seen the error with a setup which had no sink particles, amr and much larger grids and chombos.

• More time resolution than tests 2^* and 2.1^*
• particle refinement, which is faster than the amr
• again^*, dens contrast=10⁶, temp=1000K
• the disk has been rotated by theta=pi/2.
• r_disk=2 cu (=20AU; r_disk=1cu in test 2 and 2.1^*)
• disk height=2r_soft (it was .75r_soft in test2 & 2.1^*). This increase of disk height seems to reduced the length of the central warped region in comparison with tests 2 & 2.1^*.
• periodic BC (note that the domain goes from -6 to 6cu (1cu=10AU), so the disk is till far from the boundary)

The vertical expansion has a velocity ~11.4km/s, which seems reasonable.

Density movie: ​http://www.pas.rochester.edu/~martinhe/2011/binary/3feb12-955.gif

Poloidal velocity movie [mach] ​http://www.pas.rochester.edu/~martinhe/2011/binary/3feb12-1050.gif

The poloidal velocity movie shows the gas located at r ~ < rsoft is quickly pulled towards the particle. Note this is not the ambient gas. This forms a thin -2dx wide-, small central region with colliding Mach 14 flows.
Shortly after, asymmetries, likely related to grid resolution and/or numerical diffusion, develop and produce shear. The effect grows in time. This seems to cause the early central warping. It doesn't make sense to me that this central region doesn't precess; I'd expect it to rotate about the disk ang mom axis, even if at a slower speed than the Keplerian one at r >~ rsoft.		.

The fact that we see central non-precessing warping also for a disk that rotates about the x-axis (and not about the z-axis as in previous tests^*), suggests there are no grid geometry bugs. Jonathan has found the same in his own, different, exploratory central disk tests. Still I'm now running a test with an inclination angle of 10^o, as suggested by Jonathan.

It's premature to say whether this instability will affect disk material located at r >> r_soft.

^*​https://clover.pas.rochester.edu/trac/astrobear/blog/martinhe01292012

There was a meeting on Fri the 27th Jan '12. There we though about the relevant parameters for the binary simulation again.

Characteristic parameters:

• a, the separation of the stars, which we want to keep 20AU.
• AGB gravity
• AGB wind temperature, T_w
• AGB wind speed, v_w, should be ~ 20km/s
• q=M_primary/M_secondary
• gamma, which for AGB winds should be close to 1
• sigma_s= gravity softening radius of the secondary / grid resolution = r_soft/ dx
• sigma_B= gravity softening radius of the secondary / Bondi accretion radius = r_soft/r_B , where r_B=2GM_secondary/(v_w ² + c_s ² + v_secondary ²), c_s is the AGB wind's sound speed and v_secondary is the orbital velocity of the secondary with respect to the center of mass, located at the origin.

Test 1: Binaries

• Isothermal solver. It's the first time I use it for this problem
• q= 1.5, as before
• a=20AU
• T_w=1000K
• sigma_s=4cells
• sigma_B=10, i.e. 40 cells per r_B. This is accomplished with a grid of 8³ computational units with a grid of 32³+5particle refinement levels.
• v_w=20km/s
• t_final=5 orbits.

Progress:

29 Jan, 14:38. Test 1 started running on Sat the 28th morning in bluehive. I've seen some high cfl number reports after the secondary's gravity is turned on, which significantly decrease the timestep and slow the run. I've been (i) restarting with smaller cfl numbers, (ii) trying to progressively increase the secondary's gravity. The secondary has completed about .5 orbits so far. At this point, the gas that has been captured by the secondary star does not look like a disk:

I'm monitoring the progress and have 2 instances of the problem running.

30 Jan 8:15. Test1 is still running (see image), t=.8orbit. I've been finding high cfl reports which sometimes freeze the code and sometimes significantly reduce the timestep. I'm looking into the part of the code dealing with this, but in the mean time I've been running with cfls .1-.3, so the simulation is going slow. Another instance of the problem will start running in bluegene today (at some point).

The upper right panel shows a zoom of the left panel. The bottom right panel show a zoom with velocity vectors. The flow does not look like a keplerian one at this point. Seems to be early to judge whether this is correct or not.

31jan12 9:17am. InterpOrder=2. The flow does not look like a disk but we're far from 5 orbits. Compare the image to the right with the one of the 29th Jan (two above) to see the differences with the interpOrder=3 case. It's going very slow for the reasons reported in ticker167 (​https://clover.pas.rochester.edu/trac/astrobear/ticket/167) which I'm working on. In the meantime I've been running (in bluehive and have another instance of the sim waiting in bluegen's queue) with small cfls ~.09-.1.

1 Feb '12 7:55am. InterpOrder=2 continues, time=.8orbit. The flow about the secondary looks more uniform than before (see the zoomed in image →)

7 feb Running well in bluehive, 64 afrank procs. I've reduced one amr level so we can get data asap. This run includes some fixes and solver parameters that we've been discussing.

If test 1 fails (i.e. it produces a tilted or an amorphous disk) then in test 1.1 I will increase sigma_B for a fixed sigma_s. If test 1.1 fails (ditto) then in test 1.2 I will increase sigma_s and will keep everything else fixed.

Test 2: Disk at the centre of the grid

• Isothermal solver. Its the first time I will use it for this problem.
• Disk to ambient density contrast of 10⁶
• sigma_s=4cells
• extrapolated BC.

Progress.

30 Jan 8:22. Test 2 has completed 4 orbits (see images). The central part of the disk shows an inclination with respect to the orbital plane of ~ 30^o, from t=1orbit on. I do not yet understand why this happens. The outer parts of the disk remain fairly axisymmetric though. These conditions do not vary too much in time. The grid is 32³ +3amr, with a disk radius of 1 comp units.

~1 orbits
~2 orbits
~3 orbits
~4 orbits

Below is the early velocity field evolution, superimposed on the logarithmic gray scale of the density. Zoom in:

edge-on view | pole-on view

The grid seems small for the problem.

31jan12 9:17am. Here's a movie of test 2 (amr+interpOrder=3) showing the disk plane velocity field superimposed on the log(density). c_s=1. Arrows have a fixed length and are color coded.

​http://www.pas.rochester.edu/~martinhe/2011/binary/31jan12a.gif

I see: a keplerian-like vel distribution at t=0. Then there's a fast radial expansion which, I think, results from the initial pressure gradient between the disk and the amb. Would this, or a similar process, happen for IC with a disk-to-amb density contrast=1 and a super Keplerian disk vel distribution (in that case there should be no poloidal expansion though)? Then the flow still shows a velocity that scales down with r and the density seems to show some spiral-like pattern. The right panel (zoom) shows gas located well within the Bondi radius. The initial 'red' central vels seem to quickly disappear and some of the green ones do too -the central disk seems to decelerate? After such vel change, the distribution of the central disk seems to change modestly.

31jan12 10:43am. Here's a movie of test 2.1 (fixed grid+interpOrder=2). Everything is as in the movie of test 2 (above).

​http://www.pas.rochester.edu/~martinhe/2011/binary/31jan12b.gif

Group research meeting. After discussing the results of tests 2 and 2.1 we agreed I'll try:

• a colder disk, t=.1K, instead of 1000K
• taller cylindrical (not flared) disk, such that the disk height is ~ 2r_soft (it was ~.8 r_soft)
• more time resolution
• time_final=2orbits, for the warping should happen in this time.

If the above still produce warping:

• phi=pi/2, i.e. make the disk rotate about the y axis, instead of the z axis to catch potential grid related bugs
• hydrostatic disk, with no ambient medium.

Find our previous research at:https://clover.pas.rochester.edu/trac/astrobear/blog/binary

Please add more.

Theory:

Soker & Rappaport 2000 ​http://adsabs.harvard.edu/abs/2000ApJ...538..241S

Simulations:

M&M '98 (SPH) ​http://adsabs.harvard.edu/abs/1998ApJ...497..303M

Theuns (SPH) ​http://adsabs.harvard.edu/abs/1993MNRAS.265..946T

Val-Borro, Mira (2D, flash) ​http://adsabs.harvard.edu/abs/2009ApJ...700.1148D

Makita et al. 2000, 3d, plane symmetric, static disk interacting with wind ​http://adsabs.harvard.edu/abs/2000MNRAS.316..906M

3D, novae blast ​http://adsabs.harvard.edu/abs/2008A%26A...484L...9W

Close binaries:

​http://arxiv.org/pdf/astro-ph/0510175v1.pdf

​http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?2000A%26A...354.1014D&amp;data_type=PDF_HIGH&amp;whole_paper=YES&amp;type=PRINTER&amp;filetype=.pdf

Banerjee, Puldritz & Holmes 2004, simulations of collapsing, rotating Bonnor–Ebert spheres ​http://onlinelibrary.wiley.com/doi/10.1111/j.1365-2966.2004.08316.x/abstract

Observations:

Ryde et al. 2000, Mira ​http://adsabs.harvard.edu/abs/2000ApJ...545..945R

Guerrero & Miranda 2011, NGC 6778, ​http://xxx.lanl.gov/abs/1201.2042

For those of you interested in Shape and its plotting/modeling capabilities:

​http://bufadora.astrosen.unam.mx/shape/v4/screenshots/grid/screenshots.html

4 feb '12.

Three runs from the table below have completed. Bin is in the process of producing movies and plots:

​https://clover.pas.rochester.edu/trac/astrobear/blog/blin02052012

Four of the new runs (see table below) are waiting in bluegene's queue. We should have them -along with plots, diagrams, etc.- in a week time, before Adam's visit to Bruce. Additionally, Bin has 2 of these sims in the standard queue at bluehive. Note that the grid is slightly larger than before so we can see the edges of the object. Also, I have reduced 1 amr level because it adds time to the runs and post processing and doesn't give us significant info about the object's dynamics. Bruce and I have discussed about the separation of the ambient rings. The setup in runs 4, 5 and 8 (see table) seems to be consistent with the obs.

Telecon with Bruce, Adam and Jason on 26 jan '12.

• We don't need high resolution (256x128x128+2amr) to compare with the observations, which is the main objective of the paper. We will drop 1, 2 may be, refinement levels which should decrease the simulation production time.

• We don't need a constant ambient density model

• We'll do velocity and density line-outs along the jet-axis at y={-2/4,-¼,0,¼,2/4} R_clump

• We'll do PV diagrams with a slit displaced R_clump/2 from the symmetry axis

• Separation of the ambient rings form observations: ~1e16 cm = 0.9kpc*3e21cm/kpc/206265. We're using a separatin that is twice as long in the models for some experimentation showed the rings to be too close otherwise.

New simulations:

Model name	Running order	Running schedules	No. clumps	Jet	Dens contrast with ambient	Ambient	Resolution
a	1	27 Jan. Completed	1	0	200 (as the previous runs)	r-2+rings	128x80x80+2amr
b	2	27 Jan. Completed	0	1	200	r-2+rings	ditto
c	3	28 Jan. Completed	1	0	50	r-2	150x100x100+2amr
d	4	28 Jan Completed	1	0	50	r-2+rings	ditto
e	5	30 Jan Running	0	1	50	r-2	ditto
f	6	31 Jan Running	0	1	50	r-2+rings	ditto
g	7	31 Jan Queued	2; one at the initial condition and another after the 1st one has left the grid	0	50,50	r-2	ditto
h	8	1 Feb Queued	2; one at the initial condition and another after the 1st one has left the grid	0	50,50	r-2+rings	ditto

New synthetic diagrams along the correct slit position angle (turns out you cannot turn the slit in shape. The PV diagrams that I posted on Saturday correspond to a slit position angle of 0 degrees, but we want this to be 90deg. Thus I've rotated the objects with respect to the slit and had used more data from the simulations in order to see bow shocks).

Notes:

• Clump/jet are shown going up because shape's slit is like that (there's no way around this in shape. I could rotate the synthetic images later on (with gimp) for the paper versions).
• Gray scales in the left column (density maps) are logarithmic and have the same limits for all images.
• Gray scales in the emission columns (2 and 4) are logarithmic and do not have the same limits.
• Gray scales in the pv columns (3 and 5) are linear and do not have the same limits.

Clump, stratified ambient density:

Log(dens) [cm-3]	Emission (dens2) 90o	PV 90o	Emission (dens2) 60o	PV 60o

Clump, constant ambient density:

Log(dens) [cm-3]	Emission (dens2) 90o	PV 90o	Emission (dens2) 60o	PV 60o

Jet, stratified ambient density:

Log(dens) [cm-3]	Emission (dens2) 90o	PV 90o	Emission (dens2) 60o	PV 60o

Jet, constant ambient density:

Log(dens) [cm-3]	Emission (dens2) 90o	PV 90o	Emission (dens2) 60o	PV 60o

Some notes comparing Dennis et al. 2008 with our sims.

-His clump/jet vels are 100m/s. Ours are 400km/s.

-His emission and pv diagrams are for 2.5D so that's why they have more resolution, but his 3d emission maps have a little less resolution than our shape ones.

-His Fig8 is the average vx. Our vx lineouts are not averaged; they are along a single line n the x direction.

See:

​https://clover.pas.rochester.edu/trac/astrobear/blog/blin01162012

and subsequent comments.

The AAS meeting went quite well. I've got positive feedback about my talk (​http://www.pas.rochester.edu/~martinhe/austin.pdf) and chatted with most of the gang in the PN paper and with Dongsu Ryu (who invited me to give a talk in South Korea). Everyone sent greetings to Adam.

I've sent the abstract and registered for the HEDLA meeting. Adam, Eric and I should meet soon so discuss the new tower runs.

The four CRL618 runs have finished. Bin (see her post) is making movies. Do we want synthetic emission and PV diagrams of these runs?

I'm updating the PN paper. The new version will be submitted to MNRAS. I'm almost done. I should have it ready for Adam's and Eric's revision by Wednesday morning.

I'm writing the very last part of the magnetic tower paper. This is section 3.3, Energy fluxes, where we compare our calculations of the Poynting to kinetic energy ratio with those of of other flows, as requested by Pat. BTW, see ​http://arxiv.org/abs/1201.2681

The four runs (clump with a stratified ambient, clump with a constant ambient, jet with a stratified ambient and jet with a constant ambient) are all in bluegene's queue. We're also slowly pushing them forward in bluehive, but 5 amr levels require a lot of memory and computation. Here's the lates snapshot f Bin's clump-constantMedium:

yet this run, as the others did, stop do to a potential memory leak. The debugg team is aware of this and they're working on it. See

​https://clover.pas.rochester.edu/trac/astrobear/blog/blin12062011

for results of the other runs.

I've started working on this paper again. Seems to me that we have to modify:

-the abstract

-the introduction

-the conclusions

Cylindrical disks (no grav support height), gamma=1.001

Time increases downwards and the images (click to enlarge) are logarithmic edge-on views of density. Note that to have pressure equilibrium I've set temp_disk=temp_amb/100, whereas in the binary simulation these temperatures are the same. Also, in order to show as as much info about the structure of disks as possible, the color scale limits are not the same for all maps.

TABLE 1

rsoft=rd/2; rth=2rd	rsoft=rd/2; rth=8rd	rsoft=rd/2; rth=16rd	rsoft=rd/4; rth=8rd	rsoft=rd/8; rth=2rd	rsoft=rd/8; rth=8rd	rsoft=rd/16; rth=16rd
same but 2amr →	same but 2 amr →	same but 2 amr →	same but 3 amr →	same →

Flared disks (support height), gamma=1.001

TABLE 2

rsoft=rd/2; rth=2rd	rsoft=rd/2; rth=8rd	rsoft=rd/2; rth=16rd	rsoft=rd/4; rth=8rd	rsoft=rd/8; rth=2rd	rsoft=rd/8; rth=8rd	rsoft=rd/16; rth=16rd

Flared disks (support height), gamma=1.001, temp_d=temp_amb (instead of press_d=press_amb):

TABLE 3

rsoft=rd/2; rth=2rd	rsoft=rd/2; rth=8rd	rsoft=rd/2; rth=16rd	rsoft=rd/4; rth=8rd	rsoft=rd/8; rth=2rd	rsoft=rd/8; rth=8rd	rsoft=rd/16; rth=16rd

Same as table 3 (r_soft=r_d/8; r_th=8r_d) but for a Plummer gravity soft profile, instead of a spline one:

TABLE 4

Here's a movie (clock to enlarge) of the run in table 4 but with the same color bar than the corresponding column in table 3.

This is zoomed out. Note that BC are periodic:

Same as table 3 (r_soft=r_d/8; r_th=8r_d) but for gamma=1.667, instead of 1.001:

TABLE 5

We want to simulate stable Keplerian disks, here I'll keep record of the tests I'l be doing in this context.

Jonathan: So as I see it, fundamentally there are 8 different parameters that fully define the problem - at least for a fixed grid run

softening length disk height disk radius thermal radius cell size density contrast box size/boundary conditions equation of state (gamma)

I think it makes sense to fix chi >> 1 (like 100) and gamma=5/3 and to set the box length ≥ 4 disk radii to avoid boundary effects and then use periodic bc's (or reflecting)

That leaves only five parameters: softening length disk height disk radius thermal radius cell size

I think we want to keep the softening length small but not too small … Because of numerical diffusion - gravitational energy that is converted into rotational energy inside of a few cells will get converted into heat resulting in jets etc… Keeping the softening length at 4 cells will reduce this effect.

That leaves 4 free parameters disk height disk_radius thermal_radius softening length

Since there is no cooling the problem can be arbitrarily scaled so the disk radius can be fixed without loss of generality and will make setting up the data files easier.

This just leaves 3 more parameters or ratios

disk height / disk radius thermal radius / disk radius softening length / disk radius

With the disk setup - there is no pressure support in the z-direction so it might make sense to have a disk that is not a hockey puck but a rotated wedge where at any given radius, the disk mass can be balanced by thermal support.. GM/r*(h/r) ~ cs^{2 or h = cs}2 * r^{2 / GM}

This would essentially give a disk where the height is a quadratic and would be comparable to the radius at r=GM/cs^{2 (or at the thermal radius)}

This would essentially remove the disk height as a free parameter and would limit it to physically consistent values… We then just have

thermal radius / disk radius softening length / disk radius

Having the thermal radius > disk radius will prevent us from having super puffy disks and having the softening length << disk radius will allow for physically consistent disk regions…

I would suggest doing a set of runs where the thermal radius = 2, 4, 8 disk radii and the softening length = 1/16, 1/8, ¼, and ½ of the disk radius

The binary problem is producing a good looking disk after 1 orbit when using r_grav-soft=0.5:

The disks that we formed before (r_grav-soft<0.5) via wind capture looked different, i.e. didn't look completely round and showed density substructure and complex motion. The new run looks promising.

We are trying finish these simulations. Bin and I have been experiencing some problems at bluehive and bluegene. These seem independent issues and I've open tickets 162 and 163 about them. We already have a reservation in bluegene for this Wednesday to solve the problem in that cluster.

As a plan B, I've sent 4amr versions of 2 of the runs to bluehive's queue.

5 dec 11. The 4amr level simulations, clump-stratifiedAMBIENT and jet-stratifiedAMBIENT, aborted after completing ~40% of the run. They were running in 24 afrank nodes at bluehive (vmem=19000mb). Chombos at that moment are ~ 700mb. They only report:

(A)

./launch.s: line 3: 5538 Killed ./astrobear

mpirun has exited due to process rank 18 with PID 5530 on node phy089 exiting without calling "finalize". This may have caused other processes in the application to be terminated by signals sent by mpirun (as reported here).

I tried restarting but they die shortly after, and produce the above error message. I will now recompile with check flags on, which will make the runs 10 times slower but should give more info at abortion.

About the 5amr runs and bluegene. We have a reservation in that cluster for this Wednesday to do debugging.

Regarding Keplarian disks, with gamma=1.001, which move about a point gravity without any disturbance from the ambient medium. I've found a correlation between the point gravity softening radii, r_s, and the undesired disk gas motion. This is for the binary simulation setup (i.e. grid size, BC, and scales).

Basically, for 4 amr levels, disks are symmetric and stable (i.e. neither tilt nor explosion) for r_s>0.5, but unstable for smaller r_s. More exploration is needed, but thing are looking pretty good.

r=0.5 is about 3% of the grid size. The wind-capture disks that we've been seen so far had a radius close to 0.5, but his may change now with a different r_s. for 4 amr, r_s this was resolved with 8 cells

The stable disks I've been seeing have a radius of .5 too. This means that all the initial disk gas is in the flat part of the grav potential. I was using much smaller r_s because I wanted to model the grav potential as accurate as possible.

See my latest research report at: ​https://clover.pas.rochester.edu/trac/astrobear/blog/category/Meeting-outline

​https://clover.pas.rochester.edu/trac/astrobear/blog/category/Meeting-outline#martinsOutline

Summary of the Magnetic fields in the Universe III conference (​http://www.oa.uj.edu.pl/mfu2011/):

Reconnection:

-what triggers it?

-what determines its rate?

-what's the condition for fast reconnection?

-turbulence? fractal reconnection?, plasmoid-induced reconnection?

-what is its role in: MRI, star formation, dynamo, acceleration of jets?

-may reconnection jets may be observed in the ISM?

-does reconnection jet leads to shocks and possibly triggers SF (Tanuma & hibata 2007, PASJ, 59)?

-turbulent FAST reconnection

Particle acceleration:

-what are the mechanisms?

-what fraction of mag energy goes goes to non-thermal particle acceleration in reconnection?

Star formation (SF) cores: -Partially ionized phase with strong fields?

-b-fields strength and morphology in extended clouds & cores?

-diffusion mechanisms leading to SF cores?

-cloud and star formation schemes with turbulence and b-fields … the path to form clouds may be important

Milky way:

-NGC 6744 is the most similar galaxy to ours

-large scale reversals in the disk

-odd-symmetry halo fields?

-strong vertical fields in the central region

-existing fields models seem insufficient

-pulsar RM data: local fields is clock wise, but the fields in Sagittarius arm is counter-clockwise; one reversal.

-RM from background sources possibly dominated by HI structures

-field models should accept that spiral arms of the Galaxy are not regular

-the regular fields may not be located in the spiral arms

-model should include halo fields

-simple quadrupole models are wrong.

-MRI-driven dynamos. Consistent with obs?, cooling?, ionization fraction?

Galaxies

-there are halo fields (Marita Krause). Indication of galactic winds

-there are inter galactic fields and turbulent fields. Polarized radio intensity is a signature of ISM turbu.

-no dynamo without wind

-Caution: distinguish between anisotropic fields (compression or shear; stronger in density-wave galaxies) from truly regular ones.

-butterfly diagram of fields patterns from MRI models (Mami Machida). Statistics of even/odd-symmetry fields patterns are needed.

More questions:

-the golden age of polarimetry is comming.

-Key observations to be done before MFU4?

-Do we expect answers or more questions from the the SKA and LOFAR?

-ALMA will zoom in to SF cores

-SFRxMF correlation in gals. evidence of turbulent dynamo?

-origin of B in diffuse IGM (TeV - GeV obs. > 10^-16G. Seed fields of cosmological origin/phase transition or Biermann battery

-diagnostic with GENUS/TSALLIS statistics in turbulence

-reliable foreground maps based on turbulence to remove from CMB maps - PLANCK

-mean field dynamo models. realistic or not?

-stability of jets at all scales

-combine different obs. in a better way

-what theoretical work is necessary?

-what to "bridge" the gaps between theory, sims and ob?

2011. This page is a continuation of

​http://www.pas.rochester.edu/~martinhe/magneticTOWERS.html

Aug

More progress on the paper(​http://www.pas.rochester.edu/~martinhe/2011/magTOWER/paper.pdf). New azimuthal forces plot, Figure 8. Estimate 1st draft to be ready in a few weeks (before I go to Poland).

Here's the poster I'll present in Poland (​http://www.oa.uj.edu.pl/mfu2011/):

​http://www.pas.rochester.edu/~martinhe/2011/magTOWER/poster.pdf

Also, for the curious folks, here's the latex poster source code (compile with pdflatex poster.tex):

​http://www.pas.rochester.edu/~martinhe/2011/magTOWER/poster.tar

July.

Writing the first short paper about our magnetic tower simulations. Latest draft: ​http://www.pas.rochester.edu/~martinhe/2011/magTOWER/paper.pdf Currently writing the results sections.

New movies. Field line movies only show 4 lines in the central part of the tower. This makes them much clearer; using more lines make movies confusing.

Adiabatic:

• dens vs beta:

​http://www.pas.rochester.edu/~martinhe/2011/magTOWER/summer/densVSbeta-slow.gif

• field lines lateral view:

​http://www.pas.rochester.edu/~martinhe/2011/magTOWER/summer/adiabat-side-slower.gif

• field lines upper view:

​http://www.pas.rochester.edu/~martinhe/2011/magTOWER/summer/adiabat-up-slower.gif

• Three tower cases:

field lines lateral view (I tried showing the towers closer to each other and larger, but visiti does not follow my commands. I'd have to do it by hand): ​http://www.pas.rochester.edu/~martinhe/2011/magTOWER/summer/3towers-slow.gif

I will talk about my progress in the following projets (2011).

29 nov

• Magnetic tower paper. Writing the conclusions. Should have it ready for Adam's and Eric's final revision by the end of the week.

• CRL 618. The new 4 runs, with AMR (i.e. no particle grids), are in bluegene's queue. I've experienced some code running problems there, but Jonathan and I are working to solve them. In addition, Bin and I are running two of the sims in bluehive. Finish time estimation of 4 day/sim.

• Binary.

-Setup comparison:

​http://www.pas.rochester.edu/~martinhe/2011/binary/diffSETUPS.gif

I've been working on two simulations: one with an initial Keplerian disk and the other one with the orbiting binaries.

-Initial Keplerian Disks, gamma=1.001.

+5amr, no ambient wind, the disk is unstable and tilts. I'mm still running this sim further:

​http://www.pas.rochester.edu/~martinhe/2011/binary/29nov-densCONTOURS-pole.gif

​http://www.pas.rochester.edu/~martinhe/2011/binary/29nov-densCONTOURS-edge.gif

​http://www.pas.rochester.edu/~martinhe/2011/binary/29nov-densCONTOURS-angle.gif

Now trying 6amr but keeping the same gravity soft radius than in the 5amr sim.

+The disk is embedded in an abient medium with dens=dens_disk/1000 and v_x= 20kms^-1:

​http://www.pas.rochester.edu/~martinhe/2011/binary/29nova.gif

Currently running one without any wind and 5 amr levels.

-Binaries. I've ran a test simulation with the primary injecting the wind, while the secondary pulls gas form t=0 with 4amr levels. I see that a disk forms and tilts (apologies for the ugly image, the orbital plane is the XY one):

​http://www.pas.rochester.edu/~martinhe/2011/binary/29nova.png

Currently running one with 5 amr levels and a secondary's gravity field which will be tunned on once the primary's wind goes beyond the grid boundaries. Snapshot:

​http://www.pas.rochester.edu/~martinhe/2011/binary/29novf.png

21 nov

• CRL 618. New runs with diffusion and artificial viscosity seem to get rid of carbuncles. Also, seems that, as expected, 5amr, 64 cells/r_clump are necessary to resolve the clumps properly. The two movies below show runs with a density contrast of 100 and a particle grid which follows the clump or the jet.

• Clump, rho_amb=const, 4amr

​http://www.pas.rochester.edu/~martinhe/2011/crl/21nova.gif

• Clump, rho_amb=r^-1, 4amr

​http://www.pas.rochester.edu/~martinhe/2011/crl/21novd.gif

• Jet, rho_amb=const, 5amr

​http://www.pas.rochester.edu/~martinhe/2011/crl/21novb.gif

(in this test the particle is a bit offset relatie to the jet's head, this will be corrected for future runs).

• Jet, rho_amb=r^-1, 4amr. The bowshock seems too thick. I'll reduce the diffusion for the next run.

​http://www.pas.rochester.edu/~martinhe/2011/crl/21novc.gif

• Disks. I found that the latest datasets yield a stable disk at the centra of the grid with a Keplerian vel profile fir both gamma=1.001 and 1.667. I've defer a simulation which will include an inflowing wind because I want to get the binary simulations running soon for my aas talk. The binary implementation is almost ready. My tests are not long enough to see any potential disk tilt.

• Magnetic towers. New paragraph and plot (which substitutes the one I showed during the last meeting) where I quantitatively show that our towers are PFD,

see pages 21 and 23 of the latest draft:

​http://www.pas.rochester.edu/~martinhe/2011/magTOWER/paper.pdf

I plan to have the paper ready by the beginning of next week?

• PN paper. I've not yet let the other co-authors know about the latest referee's response.

What now?

Are we submitting the paper as it is now to MNRAS or New Astronomy?

• Students. Ruka has given me the 1st draft of his report.

16nov

• Students. Ruka's Bondi module is now working! (see his post). Matt's final part of the testing scripts seem to be working too. We're ready to start testing (Matt ?). We've included new tests to catch bugs related to Hypre and threading compilation flags.

• Accretion disks. My implementation keeps showing disk tilt, but velocity plots suggest it is caused by material that flows along the disk poles and collides at the centre. Even with a disk to ambient density contrast of 100 and gravity potential softening. I also tried gamma=5/3, but the disk ended up launching some sort of jet, very early in its evo.

I'm now working with Jonathan's implementation. Differences:

I see a stable disk. I'm now running two sims: one with the disk alone and one with an incoming wind too. I'll next couple Jonathan's implementation with my binary one. I expect to have this in a week time.

• Magnetic towers. New plot: Poyting to kinetic fluxes:

​http://www.pas.rochester.edu/~martinhe/2011/magTOWER/pfd.pdf

Andrea: "The pictures look fine indeed and pretty convincing. However be aware that the 1/ (beta M^{2) relation is only (very) approximative and may not apply everywhere. The only way to really show it is PDF is to calculate the Poynitng flux and kinetic flux along the jet at different height/radii and compare. I really think it is worth the effort, even for future work.".}

I'll so some plots of the ratio of Poyting to kinetic flux: [ B_z²/(8pi) ] v_z / ( .5 rho v_z³ )

• AGN jet truncation due to stellar winds. Tests keep going well. The following show an AGN radio jet with an opening angle of 20^o, and a star with a strong wind, but not so to truncate the jet.

​http://www.pas.rochester.edu/~martinhe/2011/agn/2d-dens-10nov11.gif ← small grid

​http://www.pas.rochester.edu/~martinhe/2011/agn/2d-dens-16nov11.gif ← large grid

We expect larger opening angles close to the host galaxy (​http://www.cita.utoronto.ca/~everett/agnOverview/31xopmon.jpg) and we also want the star to have some velocity and a stronger wind. Coming up soon.

• CRL 618. New implementation to follow the clump faster and see the effect of artificial viscosity, difusion and the code's limiters on the spurious features that we saw (along the head of the clump) before (see Bin's blog).

​http://www.pas.rochester.edu/~martinhe/2011/crl/16nov.png

Note that the time figures are larger by a factor of ~10 because these runs have been compiled with check flags on. Future simulations will run ~10 times faster.

Running with a massless particle allows us to make full sims in a coupe of days. Once we're happy with the diffusion setup and the morphology of the clumps, we can either switch to the gradients AMR or combine it with the particle's, in order to capture the clump/jets' cavity with higher resolution.

8nov

• Magnetic tower paper, sent to all co-authors. Got responses from Andrea and Pat. Waiting for comments from Adam, Eric and Sergey.

• Binary. 6amr run has almost completed 20 orbits, like the 5 amr one. 5+6amr run is still running.

*Disk tests. These are set up as flat (radius/height=4) cylinders at the center of the grid, with a constant disk to ambient density ratio of 10 and a Keplerian azimuthal velocity about the central, static, point gravity particle. The rest of the setup (gamma=1.001, mass_particle, grid size, scales, etc.) are as in the binary simulations (see previous posts). No wind is injected, and the duration of the movie is equivalent to 2 orbital periods of the binary simulations.

-The disk does not reach a stable state, at least for the simulations' times explored, but I'm still running these tests.

-The link below shows logarithmic density maps, upper view, of a 5amr (left part) and a 6amr (right part) disk.

​http://www.pas.rochester.edu/~martinhe/2011/binary/8nov11.5amrVS6amr.gif

-The link below shows logarithmic 3d density iso-coutours. 5amr (top) and a 6amr (bottom). Edge-on (left) and pole-on (right). The viewing position is the same in all panels; the bottom ones actually show a smaller disk. The beginning of the simulations is particularly surprising (left column) for I see oscillations of the gas that is in the central most orbits.

​http://www.pas.rochester.edu/~martinhe/2011/binary/8nov11.5amrVS6amr.3d.gif

-The initial oscillations are likely due to ambient medium which is nor rotating about the central gravity particle and is thus pulled by gravity along the poles. Also, the ambient medium and the disk have temperatures of 100 and 10 K, respectively. The idea was to have pressure equilibrium as initial conditions. Yet, may be the low temperature of the disk is such that the scale defined by the contrast of Keplerian to sound speeds is rather small and so I do not resolve it, even with 6 amr levels. This is motivated by the fact that I see the inner part of the disk very rapidly collapses in to a 2 cell thick structure. I'm now working to improve the implementation.

• CRL618. Bin and I have the new setup which includes diffusion and carbuncles prevention. Our runs (jet/clump to ambient density ratio of 100 with a constant, and stratified, density ambient) are waiting in bluehive's queue.

• AGN jet truncation due to stellar winds. Tests are going well:

​http://www.pas.rochester.edu/~martinhe/2011/agn/agn.8nov.gif

​http://www.pas.rochester.edu/~martinhe/2011/agn/agn.8nov.2.gif

This is a logarithmic false colour map of the grid gas density. The jet enters the grid on the left vertical face. The star has a spherical wind (Mdot~5e-6, v~500km/s) and is at the intersection of the three planes, at the middle of the grid. The flow structure after the collision of the stellar wind and the jet is very interesting, potentially observationally distinctive.

1 nov

* Binary.

• Tests with a simple disk about one star (only) are running (see link below, 2d slice, left: the disk just before interacting with the wind; right: the disk just after interacting with the wind). Results soon.

​http://www.pas.rochester.edu/~martinhe/2011/binary/1nov11a.png

• Soothed plots: Angm. mom. projection, mass and accretion rate (which seem to be rather high) vs time, for 5 and 6 amr levels:

​http://www.pas.rochester.edu/~martinhe/2011/binary/1nov11.pdf

25 oct

• Magnetic tower project.

*Hydro comparison: ​http://www.pas.rochester.edu/~martinhe/2011/magTOWER/25oct11.pdf.

*Working on Andrea's comments.

• Binary project.

*Run with 6amr levels is still running and it has gotten up to time=14.8 orbits. The disk tilts; I see and angle ~ 10^o-50^o between the orbital ang. mom. vector (vertical direction) and that of the disk.

*Run with 5amr unitl time=3 orbits, and then restart with 6amr levels is running too. It is rather slow though. I'm working to fix this.

*Run with 7amr unpractically slow; quite a bit of fractional steps between every level 0 step. I'm now:

*updating my implementation to use threading *running with a slightly large gravity softening radius (which will make the conditions at the inner disk less dramatic)

to see if it helps.

• CRL618 project.

*bear2fix and shape are now working. Bin's in charge of producing the synthetic emission and PV diagrams.

*Also running another clump-no rings case with more resolution at the flow behind the clump, as requested by Bruce via email.

• AGN jet truncation project. Implementing it.

18 oct

• I worked on the 3 proceeding from the magnetic fields in the universe 3 conference. I submitted them yesterday. Will post them in astro-ph this week.

• Magnetic tower. I've been writing the intro and Andrea's comments. The hydro-rotating run is in bluegene's queue. I expect to have the data in a few days time.

• Binary. We have a 5 amr and a 6amr runs. Both have completed about 10 orbits.
  • r_disk(6amr) < r_disk(5amr).
  • 6amr disk shows a rather moderate tilt, whereas the 5amr disk, as we saw before, tilts all the way to the orbital plane.
  • Projected angular momentum plots (something's wrong): ​http://www.pas.rochester.edu/~martinhe/2011/binary/18oct11.pdf
  • Density movies: ​http://www.pas.rochester.edu/~martinhe/2011/binary/18oct11.gif

Meeting resolutions: (i) continue running the 6 amr run (ii) run a 7amr version (iii) run a 5 amr until orbit 3, and then restart with 6amr (iiii) revise the angular momentum projection angles plots routine.

• CRL 618. I'm working on the synthetic maps. First test of the jet with ambient rings: ​http://www.pas.rochester.edu/~martinhe/2011/18ocr11-crl.jpg

• AGN jet truncation. I met with Eric yesterday to discuss simulations to explore ​http://adsabs.harvard.edu/abs/2006MNRAS.371.1717H. We agreed in a couple of test I'll run soon, in which a light 3D hydro jet will run into a sink particle with a spherical wind of M^.~10^-6 M_suny^-1 and v_wind~100 km s^-1.

• I'll be out of town this friday.

11 oct

• Binary wind capture problem. I've finished the Tenerife proceedings and registereed to the aas meeting in January, at TX. Since it's close to the holidays I was planning to change my plane tickets so I can aslo give some seminars at Mexico's Institutes of astronomy and astroph.

High resolution run is still running. I've found that the disk that forms has a radius about 4 times smaller than disks we've seen so far. Here's a 3D dens iso-contour snapshot after 3.5 orbits:

​http://www.pas.rochester.edu/~martinhe/2011/binary/11oct11a.png

There's a slight tilt of the disk.

Previous run: angular momentum vector projection angle plots:

​http://www.pas.rochester.edu/~martinhe/2011/binary/11oct11b.png

movie:

​http://www.pas.rochester.edu/~martinhe/2011/binary/11oct11b.gif

• Magnetic tower. I've been working on the intro of the paper. I'll then work on the rotation section to include Andrea's comments, and we should then be ready to submit.

We have enough data to make a second paper that analyses the hydro vs. PFD regimes further, as Eric has been suggesting. We should talk about that with him. i.e. how would that affect the current text. Also, I want to use the data to do some statistical analysis on synthetic polarimetry for a third paper.

I've also been writing the Poland's proceedings about the mag tower+ experiments talk. The one about the tower poster is ready.

• AGN: I've been writing the proceedings about the AGN poster that I took to Poland (​http://www.pas.rochester.edu/~martinhe/AGNposter.pdf). Ready for submission too.

• CRL 618: I've been trying to make shape synthetic emission, and PV, images. They are not ready yet, but I estimate another week for it.

• Testing: We've been having regular meetings. The RT module, data files and testing page (​https://clover.pas.rochester.edu/trac/astrobear/wiki/TestSuite/RayleighTaylor2D) are ready. Edd has also been working in documenting the FieldLoopAdvention one. Bin is working on her radiative shock bear2fix data files and in updating their documentation. Ruka's now fluently playing with the code and has started the implementation of the 2.5D hydro Bondi accretion test. Matt is working on the testing scripts. We should have the 1st version of the suite ready very soon now.

4 oct

• I've been writing the NSF proposal.

• All crl616 run complete. We should have a telecom with Bruce.

• Binary-formed accretion disk. I ran the latest simulation from longer. Another one, with an extra refinement level, is running now.

• I'm writing the Tenerife proceedings. Want to send them by Friday.

• I'm writing the AAS, TX, abstract about the binary problem.

• How's the magnetic tower paper going?

27 sep

• CRL 618. Problem: jet run is much slower than the clump one. The chombos show maxDens_clump~97, but maxDens_jet(head)~900, at t_comp~0.0084. Problem in the module. Fixed and running both jet with and without rings. Quick ugly density plots:

​http://www.pas.rochester.edu/~martinhe/27sep-crl618jets.png

• Advances in the binary problem. See Accretion-disc post.

• Working on the NSF proposal and different proceedings we have.

• Updates to the testing wiki page. Matt and I will get our hands on the testing scripts and related bear2fix routines this week.

• The hydro cooling case of the magnetic tower has completed:

​http://www.pas.rochester.edu/~martinhe/2011/magTOWER/27sep.png. The next one is the hydro rotating which I'll run soon.

20 sep

• Binary simulations. The new run, which has a grid twice as large -in every direction- than the previous run, in on going. Should have a movie for the research meeting.

• CRL 618. The clump run, with and without ambient rings, have completed (see Bin's blog). The jet runs, with and without ambient rings, are slowly on going. We should have data to show to Bruce Balick in a week time.

• Magnetic tower. Waiting for Sergey's and Andrea's comments. Writing the talk proceedings. Running (gbene) the hydro+cooling case, as requested by Eric.

• Writing the Tenerife and Poland (AGN) proceedings.

13 Sep.

• Tenerife PN proceedings?
• I have been working on:

• Binary problem, bear2fix plots of mean angular momentum vector direction vs time

• Updating testing documentation and scripts

• Matt?

6 Sep.

-Present a summary of the MfuThree meeting, and discuss about some potential collaborations with people I saw there.

-Possibly related to the magnetic tower sims:

-​http://arxiv.org/abs/0804.1871

-​http://arxiv.org/abs/0903.5340

-Discus some ideas about the binary, wind capture, accretion disk formation simulations.

-Discus about Bin's and Ruka's (the new undergrad) projects.

15 aug New initial conditions for the binary problem which seem to affect the inclination of the disk found before.

I'll present a preview of my jet Poland talk at the journal club. I'll leave this Friday and will be back on Tuesday the 30th.

Still working on the magnetic tower paper. Plan to give the 1st draft to Adam and Eric this Thursday.

27 June

Accretion disk formation ​https://clover.pas.rochester.edu/trac/astrobear/blog/category/Accretion-disk. Do the resolution and outflow radius affect the average orientation of the disk?

Magnetic tower. Paper results analysis.

Bin and I have been working on the new CRL-618 runs with velocities of 200 and 500km/s.

This page is continuation of ​http://www.pas.rochester.edu/~martinhe/2011/binary/binary.html.

Sep 27

Find movie of the disk density at ​http://www.pas.rochester.edu/~martinhe/2011/binary/27sep.gif. Top - logarithmic density maps of the orbital plane. Bottom - 3-D logarithmic density iso-contours viewed edge-on (left); y (vetical) - z (horizontal) plane -perpendicular to the orbital plane- showing linear maps of the Vz velocity component (right). The bottom right panel maintains its blue-red colors close to the left and right boundaries, hence no inflow.

The disk tilts (see bottom left panel). And the tilt angle sem to increase in time. Could this be torques from the AGB wind on the disk?

Angles plot: ​http://www.pas.rochester.edu/~martinhe/2011/binary/27sep-angles.png

Sep 23

Case with V_AGB=5km/s. This is slightly less than the scape velocity from the secondary which, thus, dominates the wind dynamics after a few orbital periods after its gravity is switched on.

Sep 22

a=25AU, V_AGB=10km/s (twice as fast as in old sims), l_grid=200AU (twice as long as the old sims), outflow_only BC. I do not see inflow from the boundaries. I see a varying tilt angle (10^o-45^o) between the disk and the orbital angular momentum vectors. ​http://www.pas.rochester.edu/~martinhe/2011/binary/22sep.png

Angular momentum projection angles plot is coming soon.

Sep 14

Some corrections to the bear2fix angular momentum projection routines. The still plots in the two links below have been updated accordingly. Mild changes. I've resumed the simulation that corresponds to the links below (a=25 AU, v_AGB=5km/s), it's running in bluehive and should go three times further.

Sep 13

Plot of the mean angular momentum direction as a function of radius and time: ​http://www.pas.rochester.edu/~martinhe/2011/binary/plot.pdf

Plot of the mean angular momentum direction as a function of time: ​http://www.pas.rochester.edu/~martinhe/2011/binary/13sep.html

Aug

a=25AU, Vagb=5km/s, "sandwich grid" (-5:5,-5:5,-2.5:2.5) AU. This simulation has two phases. During the 1st one, the binaries orbit each other twice, the AGB primary has its slow wind and the secondary only affects the orbit of the primary, but not the gas. This allows the grid to be filled with the AGB wind condition before the disk formation begins. The 2nd simulation phase begins next, when I turn on the gravity between the secondary and the gas. The system orbits 4 times.

2D pole-one logarithmic density map:

​http://www.pas.rochester.edu/~martinhe/2011/binary/25-5-fullAGB-2Ddens.gif

3D, 2 panels: pole-on and edge-on views. The disk that forms is not significantly tilted.

​http://www.pas.rochester.edu/~martinhe/2011/binary/25-5-fullAGB-2panels-3Ddens.gif

Also ran the same simulation but in a cubic grid. I see significant differences in the disks:

​http://www.pas.rochester.edu/~martinhe/2011/binary/25-5-2panels-3Ddens-sandwichVScubicGRIDS.gif

Here's a good still shot too:

​http://www.pas.rochester.edu/~martinhe/2011/binary/2panels-3Ddens-sandwichVScubicGRIDS-0180.png

A cubic grid version also with an AGB wind which has filled the grid and a=25AU, but with Vagb=30km/s, is running now. Should have the movie in a few days (before my trip).

Next simulation: a=25AU, Vagb=5km/s. The initial conditions for the disk should be an AGB wind which has expanded beyond the grid boundaries.

The simulation of a=25AU and Vagb=5km/s has run up to 5.7 orbits. Here's a number density [cm^-3] logarithmic grayscale map, and an opaque dark-blue map of the grid:

​http://www.pas.rochester.edu/~martinhe/2011/binary/25-5-2Ddens.gif (A)

The grid in this simulation is [-5:5,-5:5,-2.5:2.5], "a sandwich", and each computational length unit=10AU. This makes the simulation faster without compromising disk formation dynamics. I see complex flow patterns. The rotation of the diks is synchronous with the orbital one.

Here a 3D view of the number density of this simulation:

​http://www.pas.rochester.edu/~martinhe/2011/binary/25-5-2panels-3Ddens.gif (B)

The left panel is a perspective view. The AGB primary is the red particle. The orbital plane is opaque, in the middle of the figures. This is a viewing angle of about 10 degrees. Disk material below the orbital plane is shaded. The right panel shows the same simulations but normal to the orbital plane and from bottom to top relative to the left panel.

Newest runs (as fas as they've gotten). a=binary separation [AU] , v=AGB [km/s] wind velocity.

a=5, v=5. ​http://www.pas.rochester.edu/~martinhe/2011/binary/summer/18jul-densISOCONTOURS-a.gif

a=5, v=30. ​http://www.pas.rochester.edu/~martinhe/2011/binary/summer/18jul-densISOCONTOURS-b.gif

a=25, v=5. Tired to run with lScale=10AU and the same grid size as the tow simulations above (just at the post of 13 june, ​http://www.pas.rochester.edu/~martinhe/2011/binary/binary.html). This setup, however, produced wrongly high v, because the code's velocity scale only depends on tempScale (i.e. velscale \propto tempscale and not to lscale). Easy solution would be to reduce tempscale and rerun. Yet, I decided to change as little parameters as possible between different runs (a=5 and a=25), so I'm now running this case (a=25 v=5) with lscale =1AU and a 4 times larger grid than in the a=5 case. Progress, about .5 orbit.

a=25, v=30. Very problematic run. Need to adjust AR to follow the wind while it travels between the stars. Currently running in bluehive with the above described setup. Progress, I only have 3 chombos, ~ ¼ of the 1st orbit.

Difficult to get much further before the Tenerife conference.