Summary
This model has an initial resolution of about 0.01 pc and a finest grid after zooming of about 200 AU. The magnetic field is initially on the order of 10-25 $\mu G$.
Simulated using Ramses 3 (MHD)
Parameters
Parameter | Value |
---|---|
boxlen_pc | $66.0948$ |
cont | 10. !density contrast |
ff_rt | 0.0 !freefall time/rotation time |
ff_sct | 0.07 !freefall time/sound crossing time |
mass_c | 100000. !in solar mass |
rap | 2.5 !axis ratio |
time_Myr | $0.672096$ |
Tsat | $1000000$ |
boxlen_codeunits | $66.2167$ |
boxlen | 66.2167 |
cooling | |
courant_factor | $0.8$ |
gamma | $1.66667$ |
hydro | |
jeans_refine | 25*10. ! Allow Jeans refinement anywhere |
levelmax | $16$ |
levelmin | $8$ |
n_sink | 1d8 |
ncpu | $672$ |
nexpand | $1$ |
nstep_coarse | $1000$ |
nsubcycle | 3*1,10*2 |
pic | |
poisson | |
pressure_fix | |
r_refine | 10*0.95 ! FIRST TWO LEVELS MUST REFINE, THEN JEANS REFINEMENT |
riemann | 'hlld' |
riemann2d | 'hlld' |
sink | |
slope_type | $1$ |
time | $0.00835191$ |
unit_d | $2.32474e-24$ |
unit_l | $203947283049999990784$ |
unit_t | $2539507900000000$ |
x_refine | 10*0.5 |
y_refine | 10*0.5 |
z_refine | 10*0.5 |
Applied physics
- Self-gravity
- Self-Gravity is applied.
- Star formation
- Star formation is treated using Lagrangian sink particles that accrete the surrounding gas and interact gravitationally with it.
- Hydrodynamics
- Hydrodynamical equations are solved
- Magnetohydrodynamics
- Ideal magneto-hydrodynamics is resolved.
- Supernovae feedback
- No supernovae feedback
Snapshots
ORION_00005 (t=$0.672096 \; \textrm{kyr}$)
descrip_snapshot
Catalogs :
Datafiles:
ORION_00009 (t=$0.769059 \; \textrm{kyr}$)
descrip_snapshot