1D, 2D and 3D collapse of interstellar clouds

Details 1D, 2D and 3D collapse of interstellar clouds 1D, 2D and 3D collapse of interstellar clouds

Dec 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980ssrv...27..235t&link_type=abstract

(International Astronomical Union, Colloquium on Stellar Hydrodynamics, 58th, Los Alamos, N. Mex., Aug. 12-15, 1980.) Space Scie

Physics

12

Cloud Physics, Gravitational Collapse, Interstellar Gas, Stellar Evolution, B Stars, Early Stars, O Stars, Protostars, Stellar Luminosity, Stellar Models

Scientific paper

Recent theoretical investigations and numerical models of star formation with various symmetries (one-dimensional or spherically symmetric, two-dimensional or axisymmetric, and three-dimensional) are reviewed. Observations strongly suggest that stars condense out of cool (about 10 K) and dense (1000-10,000 atoms/cu cm) interstellar clouds due to gravitational instability and collapse. Bright young stellar objects (O and B stars) are always found in the vicinity of cloud complexes.

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