Rotation-dominant equilibria of isothermal clouds

Details Rotation-dominant equilibria of isothermal clouds Rotation-dominant equilibria of isothermal clouds

May 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990mnras.244..349n&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 244, May 15, 1990, p. 349-356.

Statistics

Computation

6

Computational Astrophysics, Gravitational Collapse, Rotating Bodies, Star Formation, Density Distribution, Integral Equations, Pressure Distribution

Scientific paper

Rotating isothermal clouds in equilibrium are classified into two groups: one is in the pressure-dominant (PD) state and the other in the rotation-dominant (RD) state. All the numerical solutions obtained so far, however, belonged essentially to the former group. It is found that the latter solutions cannot be obtained as far as the self-consistent-field method of Ostriker and Mark is employed in computation. In order to investigate whether or not the RD equilibrium state can be attained at the end of the collapse of rotating clouds, the RD solutions are obtained under a thin disk approximation using a new numerical method.

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