Collapse and equilibrium of rotating, adiabatic clouds

Details Collapse and equilibrium of rotating, adiabatic clouds Collapse and equilibrium of rotating, adiabatic clouds

Dec 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...242..699b&link_type=abstract

Astrophysical Journal, Part 1, vol. 242, Dec. 1, 1980, p. 699-709.

Other

40

Adiabatic Conditions, Gravitational Collapse, Interstellar Gas, Main Sequence Stars, Stellar Evolution, Stellar Winds, Computer Programs, Dynamic Stability, Equations Of Motion, Poisson Equation, Stellar Rotation

Scientific paper

A numerical hydrodynamics computer code analysis of the collapse and establishment of equilibrium of adiabatic gas clouds restricted to axial symmetry found that the clouds are originally uniform in density and rotation. The method can compare the dynamic collapse and approach to equilibrium with the data on incompressible uniformly rotating equilibrium clouds and on equilibrium structures of differentially rotating polytropes. It is concluded that the stellar formation theory indicates that the low alpha fragments produced at the termination of the dynamic isothermal collapse phase of interstellar clouds may undergo significant dynamic collapse in an adiabatic regime leading to transitory ring formation and additional fragmentation on a smaller scale.

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