Documents and Papers

1. ​Stone&Proga 2009
2. ​Matsakos, Uribe & Königl 2015
3. ​Matt & Balick 2004
4. ​Matt & Pudritz 2008
5. ​Cohen et al 2009
6. ​Cohen et al 2011
7. ​Borrier et al 2013

Paper Figures

1. ​Pictures for Paper IAU 314
2. ​Pictures for Paper Interaction

Co-rotating Parameters

1. ​Parameters Comparing with Matsakos
2. ​Parameter Space

Simulation and Restuls

4.15.2015

1. Parameters

Check blog:afrank04152015 for details

Hot Jupiter

M_{p} = M_j

R_{p} = R_j

n_{p} = m_h

T_{p0} = 10^4

Stellar Wind

V_{s} = 100 km/s

Other parameters.

Resolution: 60 zone/planet radius -check

Allow planetary wind to fill grid for 2 of its own crossing times ( L_grid/V_pw(max) ) then turn on stellar wind and let it run for 10 crossing times ( L_grid/V_s )

2. Check lambda — no stellar wind

Rp=Outflow radius + thickness !! where the radius defines the location of boundary and thickness for wrapping up the velocity

ns/np=1e-4 gamma = 1.01;

lambda=2.6	Mp = 0.5 Mj	Rp = 2Rj	Tp=2e4	namb=1e-4	​low res movie	​high res movie	; ​zoomed high res movie
lambda=5.3	Mp = 0.5 Mj	Rp = 2Rj	Tp=1e4	namb=1e-4	​low res movie	​high res movie
lambda=5.3	Mp = 0.5 Mj	Rp = 2Rj	Tp=1e4	namb=1e-5		​high res movie	;;​zoomed in high res movie
lambda=5.3	Mp = 0.5 Mj	Rp = 2Rj	Tp=1e4	namb=1e-6		​high res movie
lambda=5.3	Mp = 0.5 Mj	Rp = 2Rj	Tp=1e4	namb=1e-8		​high res movie
lambda=5.3	Mp = 1 Mj	Rp = 4Rj	Tp=1e4	namb=1e-4	​low res movie
lambda=10.6	Mp = 1 Mj	Rp = 2Rj	Tp=1e4	namb=1e-4	​low res movie	​high res movie
lambda=10.6	Mp = 0.5 Mj	Rp = 1Rj	Tp=1e4	namb=1e-4	​low res movie
lambda=10.6	Mp = 0.5 Mj	Rp = 2Rj	Tp=5e3	namb=1e-6			Tamb=1000; ​zoomed in movie

3. Backflow check for different line width of line plot — positive value means back flow

Flux=\int_{0}^{L} 2\pi x\rho(x) v_{y}(x) dx Where L is the width of line plot for the integrate.

	flux Vs time	Relative flux Vs lambda
L= 0.5 Rp at y=1.0 Rp
L = 1 Rp at y=1.0 Rp

at different positions

;

4. Runs and Results

Mp=0.5; Rp=2; lambda=5.3

#	gamma	Solar Wind Mach #	n_s/n_p
1	1.01	0.8	10-4	​low res 2.5D	​high res 2.5D
2	1.01	0.8	10-4
3	1.3	0.8	10-4	​low res 2.5D namb=1e-4;​low res 2.5D namb=1e-5;​low res 2.5D namb=1e-8;	transfering
4	1.3	0.8	10-4
5	1.01	5.0	10-4	​low res 2.5D	​high res 2.5D
6	1.01	5.0	10-4
7	1.01	5.0	10-5	​low res 2.5D;​low res 2.5D large	​high res 2.5D
8	1.01	5.0	10-3	​low res 2.5D namb=1e-5	to be analyzed
9	1.3	5.0	10-4	​low res 2.5D namb=1e-5;​low res 2.5D namb=1e-6	​high res 2.5D
10	1.01	0.8	10-3	​low res 2.5D namb=1e-5;	analyzing

5. New runs

blog:afrank04272015

Mp=0.5Mj; Vs=100km/s; namb=1e-6; lambda=5.3

#	gamma	Solar Wind Mach #	n_s/n_p	Tp	Ts	low-res results	high-res results
1	1.01	0.8	10-5	1E4 K	1.86E+6 K	​low res 2.5D Tamb=0.01K small box; ​low res 2.5D Tamb=0.01K large box;​low res 2.5D Tamb=1000K;	; ​high res 2.5D new runs 128 frames;	|
2	1.01	5.0	10-5	1E4 K	47632.6 K		;​high res 2.5D Tamb=0.01K;
3	1.3	0.8	10-5	1E4 K	1.45E+6 K	​low res 2.5D, Tamb=0.01K;​low res 2.5D, Tamb=1000K;	; ​high res 2.5D Tamb=1000K;
4	1.3	5.0	10-5	1E4 K	37006.8 K	​low res 2.5D Tamb=0.01K; ​low res 2.5D Tamb=1000K;	; ​Zoomed high res 2.5D Tamb=1000K;​Zoomed high res shorter version Tamb=1000K;

6. 3D runs

Mp=0.5Mj; Vs=100km/s; namb=1e-6; lambda=5.3

#	gamma	Solar Wind Mach #	n_s/n_p	Tp	Ts	low-res results	high-res results
1	1.01	0.8	10-5	1E4 K	1.86E+6 K	​low res 3D rho;​low res 3D T; ​low res 3D vol rendering;
2	1.01	5.0	10-5	1E4 K	47632.6 K	​low res 3D rho;​low res 3D T; ​low res 3D vol rendering;	​high res rho up to 185 frames; ​high res 3D vol rendering; ​high res zoomed rho up to 185 frames; ;
3	1.3	0.8	10-5	1E4 K	1.45E+6 K	to be analyzed?
4	1.3	5.0	10-5	1E4 K	37006.8 K	to be analyzed?

7. Rotating runs

Mp=0.5Mj; Vs=100km/s; namb=1e-6; lambda=5.3; star mass ~1 solar mass? distance between planet and star ~0.1AU, orbital angular velocity of the planet ~0.572 in C.U.

angular velocity of the Earth (1 AU from the sun: ~2.0E-7 rad/s
angular velocity of the planet (~0.1AU from the sun): sqrt(1000)*2E-7 = 6.62E-6 rad/s
time scale: 86400
angular velocity of the planet in C.U.: 6.62E-6 * 86400 = 0.572

In the co-rotating frame the stellar wind density if proportional to 1/r^{2}. where r is about 200 C.U. So to make the stellar wind density same as in the 2.5D and 3D we have to set it 40000 times larger in these co-rotating runs.

#	gamma	Solar Wind Mach #	n_s/n_p	Tp	Ts	low-res results	high-res results
1	1.01	0.8	10-5	1E4 K	1.86E+6 K
2	1.01	5.0	10-5	1E4 K	47632.6 K	​omega=0.5 small box;​omega=0.5 large box;	; ​omega=0.5 high res larger window; ​omega=0.5 3D vol rendering; ​Three sects; ​omega=0.5 new refinement 16 zone per radius;
3	1.3	0.8	10-5	1E4 K	1.45E+6 K
4	1.3	5.0	10-5	1E4 K	37006.8 K

8. Movies

1) Table 2. Row 3.  Both zoomed and unzoomed movies
2.) Table 5. #1, # 2 and #4 (Zoomed in version for #4)
3.) Table 6. #2 all 3 movies (what happens with the "pulsing" of the pwind?)
4) Table 7. #2.  Whatever we have.  Cuts and Volume rendering.

	avi	mov	mp4	mpeg
1)	​avi un-zoomed;​avi zoomed;	​mov un-zoomed;​mov zoomed;	​mp4 un-zoomed;​mp4 zoomed;	​mpeg un-zoomed;​mpeg zoomed;
2)	​#2; ​#4;	​#1; ​#2; ​#4; ​#4 shorter version;	​#2; ​#4;	​#2; ​#4;
3)	​Tri-section;	​Tri-section; ​zoomed Tri-section; ​3D volume rendering;
4)		​1 section; ​tri-section; ​3D volume rendering; ​low res very large window;

Debugging Co-rotating Frame

​check details here