The fragmentation of molecular clouds. II - Gravitational stability of low-mass molecular cloud cores

Details The fragmentation of molecular clouds. II - Gravitational stability of low-mass molecular cloud cores The fragmentation of molecular clouds. II - Gravitational stability of low-mass molecular cloud cores

Sep 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...183...98c&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 183, no. 1, Sept. 1987, p. 98-108.

Astronomy and Astrophysics

Astrophysics

31

Equations Of State, Gravitation, Molecular Clouds, Star Formation, Astronomical Models, Fragmentation, Hydrostatics, Temperature Profiles, Thermal Instability

Scientific paper

The gravitational stability of hydrostatic molecular clumps is analyzed in terms of the ambient radiation and pressure fields which vary drastically inside a molecular complex. Using a realistic equation of state for molecular gas, a large grid of self-gravitating spherical models is constructed and the stability of these models against their normal radial eigen modes is analyzed. The objective of this study is to provide the basis of an initial mass function of individual clumps on the verge of star formation. High mass pre star-forming cores are predicted to be found at the edges of 200-500 solar masses clumps, while the inner regions embody the typical cores with M less than or equal to 1 solar mass. Growing observational evidence for low mass stars clusters in evolved clouds give further impulse to an evolutionary sketch for molecular clouds and time stretching bimodal star formation.

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