Collapse and formation of stars

Details Collapse and formation of stars Collapse and formation of stars

Jan 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985sciam.252...40b&link_type=abstract

Scientific American (ISSN 0036-8733), vol. 252, Jan. 1985, p. 40-45.

Computer Science

4

Cosmic Dust, Gravitational Collapse, Rotating Matter, Solar System, Stellar Evolution, Stellar Models, Angular Momentum, Binary Stars, Nebulae, Optical Thickness, Protostars, Quasi-Steady States, Radiative Transfer, Stellar Mass Accretion, Thermodynamics

Scientific paper

The results of high-speed computer simulations of the collapse of molecular hydrogen clouds to form individual stars or multiple star systems are discussed. The process of collapse of spherically symmetric, nonrotating clouds, spherically symmetric, rotating clouds, and asymmetric rotating clouds is described, emphasizing cloud fragmentation and the transfer outward of angular momentum. The possibility that the solar system may have developed from an extremely slowly rotating cloud is considered.

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