Collapse, equilibrium, and fragmentation of rotating, adiabatic clouds

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

Dec 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980ssrv...27..255b&link_type=abstract

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

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2

Adiabatic Conditions, Dynamic Stability, Gravitational Collapse, Interstellar Matter, Molecular Clouds, Stellar Evolution, Gas Density, Main Sequence Stars, Protostars, Rotating Fluids, Thermal Energy

Scientific paper

Numerical calculations of the collapse of adiabatic clouds from uniform density and rotation initial conditions show that when restricted to axisymmetry, the clouds form either near-equilibrium spheroids or rings. Rings form in the collapse of low thermal energy clouds and have a ratio of rotational kinetic energy to the absolute value of gravitational potential energy greater than approximately 0.43. When the axisymmetric constraint is removed and an initial m = 2 density variation is introduced, clouds either collapse to form near-equilibrium ellipsoids or else fragment into binary systems through a bar phase. Ellipsoids form in the collapse of high thermal energy clouds and have a rotational kinetic energy/absolute value of gravitational potential energy ratio less than approximately 0.27. The results are consistent with the critical values of the rotational kinetic energy/absolute value of gravitational potential energy ratio for instabilities in Maclaurin spheroids, and suggest that protostellar clouds may undergo a dynamic fragmentation in the nonisothermal collapse regime.

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