Protostellar formation in rotating interstellar clouds. I - Numerical methods and tests

Details Protostellar formation in rotating interstellar clouds. I - Numerical methods and tests Protostellar formation in rotating interstellar clouds. I - Numerical methods and tests

Mar 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...236..619b&link_type=abstract

Astrophysical Journal, Part 1, vol. 236, Mar. 1, 1980, p. 619-627.

Statistics

Computation

39

Gravitational Collapse, Hydrodynamics, Interstellar Gas, Protostars, Stellar Evolution, Computational Fluid Dynamics, Euler Equations Of Motion, Gravitational Fields, Poisson Equation

Scientific paper

Attention is given to numerical methods and tests of a series of gravitational hydrodynamics computer codes constructed in order to numerically follow the dynamic collapse of spherically symmetric (1-D), axisymmetric (2-D), and non-axisymmetric (3-D) isothermal interstellar clouds. A spherical harmonic expansion is used to solve the Poisson equation for the gravitational potential. It is shown that the use of explicit donor-cell hydrodynamics on a moving spherical coordinate grid ensures mass and momentum conservation and allows the grid to follow the collapse of the fluid. Finally, the performance of the codes is examined.

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