On the Density Distribution in Star-forming Interstellar Clouds
Abstract
We use deep adaptive mesh refinement simulations of isothermal self-gravitating supersonic turbulence to study the imprints of gravity on the mass density distribution in molecular clouds. The simulations show that the density distribution in self-gravitating clouds develops an extended power-law tail at high densities on top of the usual lognormal. We associate the origin of the tail with self-similar collapse solutions and predict the power index values in the range from -7/4 to -3/2 that agree with both simulations and observations of star-forming molecular clouds.
- Publication:
-
The Astrophysical Journal
- Pub Date:
- January 2011
- DOI:
- 10.1088/2041-8205/727/1/L20
- arXiv:
- arXiv:1007.2950
- Bibcode:
- 2011ApJ...727L..20K
- Keywords:
-
- ISM: structure;
- methods: numerical;
- stars: formation;
- turbulence;
- Astrophysics - Galaxy Astrophysics
- E-Print:
- 5 pages, 3 color figures