Summary
This model has an initial resolution of about 0.01 pc and a finest grid after zooming of about 100 AU. Magnetic field is not considered.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 | 1.16985 |
boxlen_codeunits | 66.2167 |
cooling | .true. |
boxlen | 66.2167 |
courant_factor | 0.8 |
gamma | 1.66667 |
hydro | .true. |
jeans_refine | 25*10. ! Allow Jeans refinement anywhere |
levelmax | 17 |
levelmin | 9 |
n_sink | 1d9 |
ncpu | 512 |
nexpand | 1 |
nstep_coarse | 1600 |
nsubcycle | 3*1,10*2 |
pic | .true. |
poisson | .true. |
pressure_fix | .true. |
r_refine | 10*0.95 |
riemann | 'hlld' |
riemann2d | 'hlld' |
sink | .true. |
slope_type | 1 |
time | 0.0145374 |
unit_d | 2.32474e-24 |
unit_l | 203947283049827991552 |
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_00066 (t=$1.16985 \; \textrm{kyr}$)
descrip_snapshot
Datafiles:
Column density along the z-direction
Density in the xy-plane. The arrows represent the velocity field in the xy plane.
Temperature in the xy-plane.
Column density along the y-direction.
Density in the xz-plane. The arrows represent the velocity field in the xz-plane.
Temperature in the xz-plane.
Column density along the x-direction.
Density in the yz-plane. The arrows represent the velocity field in the yz-plane.
Temperature in the yz-plane.
Column density along the z-direction
Density in the xy-plane. The arrows represent the velocity field in the xy plane.
Temperature in the xy-plane.
Column density along the y-direction.
Density in the xz-plane. The arrows represent the velocity field in the xz-plane.
Temperature in the xz-plane.
Column density along the x-direction.
Density in the yz-plane. The arrows represent the velocity field in the yz-plane.
Temperature in the yz-plane.
Mass weighted density PDF.
Volume weighted density PDF.
Mass weighted temperature.
Mass weighted Mach number.
Mass weighted bidimentional histogram of the temperature vs density
ORION_00087 (t=$1.26079 \; \textrm{kyr}$)
descrip_snapshot
Datafiles:
Column density along the z-direction
Density in the xy-plane. The arrows represent the velocity field in the xy plane.
Temperature in the xy-plane.
Column density along the y-direction.
Density in the xz-plane. The arrows represent the velocity field in the xz-plane.
Temperature in the xz-plane.
Column density along the x-direction.
Density in the yz-plane. The arrows represent the velocity field in the yz-plane.
Temperature in the yz-plane.
Column density along the z-direction
Density in the xy-plane. The arrows represent the velocity field in the xy plane.
Temperature in the xy-plane.
Column density along the y-direction.
Density in the xz-plane. The arrows represent the velocity field in the xz-plane.
Temperature in the xz-plane.
Column density along the x-direction.
Density in the yz-plane. The arrows represent the velocity field in the yz-plane.
Temperature in the yz-plane.
Mass weighted density PDF.
Volume weighted density PDF.
Mass weighted temperature.
Mass weighted Mach number.
Mass weighted bidimentional histogram of the temperature vs density