BUBBLES IN THE ISOLATED GALAXY (i.e. NGC 4472 without circumgalactic gas)
These bubbles are calculated in RZ coordinates. The grid is uniform for R,z<50 kpc, with a grid size Delta z = Delta R = 125 pc. Beyond 50 kpc, the grid size increases geometrically to the boundary, placed at R = z = 260 kpc.The heating term is Gaussian (see our last heating paper, astro-ph/0301283) with a lengthscale r_h. The heating power is H (erg/s).
Before to apply the heating, at t=13 Gyr, I remove the (unphysical) cooled gas accumulated in the very center. The heating is usually applied for t_h = 50 Myr, but I have run models with t_h=100 Myr.
The initial conditions are those of the standard cooling flow (q=0) at t=13 Gyr (the one in cutden.dat). All the cooling flow ingredient are considered (alpha_*, alpha_sn) but NOT the radiative cooling.
Below are some images of the density distribution. The axes units are kpc, the time is indicated in the upper right corner, remember that heating starts at t=13.0 Gyr.
Model 1:
H=2.5e42 erg/s, r_h=1 kpc, t_h=50 Myr.
alpha_* and alpha_sn vary with time in the standard way.
Model 2:
H=2.5e42 erg/s, r_h=1 kpc, t_h=100 Myr.
Model 3:
H=5e42 erg/s, r_h=1 kpc, t_h=50 Myr (4-bubbles model!).
Model 4:
H=5e42 erg/s, r_h=2 kpc, t_h=50 Myr.
Model 5:
H=5e42 erg/s, r_h=0.5 kpc, t_h=50 Myr.
