### Summary

This model has an initial magnetic field of about 3$\mu G$ and a uniform resolution of $512^{3}$ grid points. This corresponds to a spatial resolution of about 2 pc. This run is described in Iffrig & Hennebelle 2017, A&A, 604, 70.Simulated using Ramses 3 (MHD)

### Parameters

Parameter | Value |
---|---|

Height0 | 150 |

boxlen_pc | 998.16 |

bx_bound | 0.5 |

boxlen | 1000 |

by_bound | 0 |

bz_bound | 0 |

dens0 | 1.5 |

supernovae | .true. |

time_Myr | 50.2147 |

turb | 5 |

Tsat | 1.d5 |

boxlen_codeunits | 1000 |

cooling | .true. |

courant_factor | 0.8 |

eff_sn | 0.2 |

feedback_sink | .true. |

gamma | 1.66667 |

gravity_type | -1 |

hydro | .true. |

isothermal | .false. !.true. |

levelmax | 9 |

levelmin | 9 |

n_sink | 1.d3 |

ncpu | 288 |

nexpand | 1 |

nstep_coarse | 11600 |

nsubcycle | 7*1 |

pic | .true. |

poisson | .true. |

pressure_fix | .true. |

riemann | 'hlld' |

riemann2d | 'hlld' |

sink | .true. |

slope_type | 1 |

smallc | 0.01 |

smallr | 0.0001 |

time | 0.624001 |

unit_d | 2.32474e-24 |

unit_l | 3080000000000000000000 |

unit_t | 2539507940032080 |

vsat | 200 |

### Applied physics

- Self-gravity
- Self-Gravity is applied.
- Hydrodynamics
- Hydrodynamical equations are solved
- Magnetohydrodynamics
- Ideal magneto-hydrodynamics is resolved.
- Supernovae feedback
- Supernovae feedback is applied around the densest cell in the simulation at a rate equal to the Milky way rate.

### Snapshots

#### LS_00060 (t=$50.2147 \; \textrm{kyr}$)

descrip_snapshot

##### Datafiles:

Density weighted integrated magnetic intensity along the z-direction. The arrows represent the projected direction of the integrated B in the xy-plane.

Cut of the magnetic intensity in the xy-plane. The arrows represent the projected direction of B in the xy-plane.

Density weighted integrated magnetic intensity along the y-direction. The arrows represent the projected direction of the integrated B in the xz-plane.

Cut of the magnetic intensity in the xz-plane. The arrows represent the projected direction of B in the xz-plane.

Density weighted integrated magnetic intensity along the y-direction. The arrows represent the projected direction of B in the yz-plane.

Cut of the magnetic intensity in the yz-plane. The arrows represent the projected direction of B 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

Volume weighted magnetic intensity.

#### LS_00110 (t=$74.7361 \; \textrm{kyr}$)

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.

Mass weighted density PDF.

Volume weighted density PDF.

Mass weighted temperature.

Mass weighted Mach number.

Mass weighted bidimentional histogram of the temperature vs density

Volume weighted magnetic intensity.