5/13/02

This directory contains the run with eta_*=1, B_pole=295G,
gamma=5/3. I initialzed  it with the final state
from the isothermal run with the same parameters.
T_eff=45000 K, a_iso=26 km/s was assumed.

animations:
1. adiab-295g-xray.avi-
Xray emission related to density square w/
xray=log (\rho^2 10^{-5e6/T}.
Relative values are important.

2.adiab-295g-speed.avi-
Speed of the wind flow w/
speed=\sqrt{v_\theta^2+ v_r^2}

3.adiab-295g-pbvpram.avi-
the ratio between magnetic over ram pressure w/
pbvpram= P_B/P_ram= (B^2/8\pi)/(\rho speed^2)

4.adiab-295g-pthvpram.avi-
Thermal pressure over ram pressure, 
pthvpram=P_thermal/P_ram= (\rho kT/\mu)/(\rho speed^2)
where \mu= mean atomic weight = 0.6 m_H.

5.adiab-295g-pbvptot.avi
Magnetic pressure over total gas pressure,
eta= P_B/(P_ram+P_thermal)

6.adiab-295g-rho.avi
log of density ,
d=log(\rho)

7.adiab-295g-mach.avi
Local mach number,
mach=flow speed/sound speed= speed/(1.17e7*\sqrt(T/1e6)).
[I remember that for the sun 1e6 K corresponds to 
the sound speed of 117 km/s )

8.adiab-295g-T.avi
T=log(Temperature)
Very high T material is essentially vacuum.

9.adiab-295g-benergy.avi
Just for fun I plotted magnetic energy density over its initial value,
binit= B(t)^2/B(t=0)^2

10.adiab-295g-massflux.avi
Mass flux vectors defined as,
{mx}={vx}*\rho
{my}={vy}*\rho
difficult to see, so I plotted also w/ uniform mass flux
vectors that gives a sense of which direction
the flow is moving.


11.adiab-295g-pth.avi
pth=log(P_thermal)

12.adiab-295g-gline.avi
Radial line force.
Forgot to compute gline for the initial condition.
I wonder why it was not carried over from the restart file,
need to check ZEUS for this. This should not affect the 
computation since gline is called at every iteration.

13. dib-295g-glcon.vi
In order to have a quantity that is fairly constan,
we plot 
glcon=\rho v * r^4 gline.
The rationale is:
gline ~ GM/r^2 and \rho * v ~ 1/r^2.
I should have used v=v_radial but I used v=speed, which
is good to the first approximation.