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Martin's update, 6 mar '12
-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. | 
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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/Ncells) SUMx,y,z [ fP(x,y,z,t)/fk(x,y,z,t) ], (1)
where x,y,z are cells inside boxes which contain:
- (i) the jet (RIGHT PANEL; x,y ⇐ |rjet|; z⇐ heightcavity)
- (ii) the whole magnetic cavity (LEFT PANEL; x,y ⇐widthcavity; z⇐ heightcavity).
The time averages of the above:
SUMt { (1/Ncells) SUMx,y,z [ fP(x,y,z,t)/fk(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.
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-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
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