Simulation of the Gravitational Collapse and Fragmentation of Rotating Molecular Clouds

Details Simulation of the Gravitational Collapse and Fragmentation of Rotating Molecular Clouds Simulation of the Gravitational Collapse and Fragmentation of Rotating Molecular Clouds

2005-06-08

arxiv.org/abs/astro-ph/0506174v1

2005, KFNT Suppl. Ser., N5, p. 216 - 223

Astronomy and Astrophysics

Astrophysics

8 pages, 9 EPS figures, special forma.cls class file is used

Scientific paper

In this paper we study the process of the subsequent (runaway) fragmentation of the rotating isothermal Giant Molecular Cloud (GMC) complex. Our own developed Smoothed Particle Hydrodynamics (SPH) gas-dynamical model successfully reproduce the observed Cloud Mass-distribution Function (CMF) in our Galaxy (even the differences between the inner and outer parts of our Galaxy). The steady state CMF is established during the collapse within a free-fall timescale of the GMC. We show that one of the key parameters, which defines the observed slope of the present day CMF, is the initial ratio of the rotational (turbulent) and gravitational energy inside the fragmented GMC.

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