On the fragmentation of differentially rotating clouds

Details On the fragmentation of differentially rotating clouds On the fragmentation of differentially rotating clouds

Aug 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983mnras.204..715g&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 204, Aug. 1983, p. 715-733.

Astronomy and Astrophysics

Astronomy

72

Clouds, Interstellar Gas, Rotating Matter, Rotation, Stellar Evolution, Angular Momentum, Angular Velocity, Astronomical Models, Fragmentation, Viscosity

Scientific paper

The collapse of a cloud is numerically simulated with constant angular velocity and distance from the rotation axis decreasing with distance from the rotation axis, and it is shown that intense rings can form. The particle method SPH is used in a form which, for inviscid flow, conserves total linear and angular momentum exactly. It is shown that for inviscid flow the local transport of angular momentum is very accurate. A standard three-dimensional algorithm is used to test the transport of velocity, and the various evolution sequences for a uniformly rotating and a differentially rotating cloud are described. The cases of no artificial viscosity, artificial viscosity in the z-direction only, and artificial viscosity acting on all momentum components are considered.

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