On the Density Distribution in Star-forming Interstellar Clouds

Details On the Density Distribution in Star-forming Interstellar Clouds On the Density Distribution in Star-forming Interstellar Clouds

2010-07-17

arxiv.org/abs/1007.2950v3

ApJL, 727, L20, 2011

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

5 pages, 3 color figures; published version

Scientific paper

10.1088/2041-8205/727/1/L20

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.

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