A finite-difference adaptive grid method for computing the equilibria of rotating self-gravitating barotropic gases

Details A finite-difference adaptive grid method for computing the equilibria of rotating self-gravitating barotropic gases A finite-difference adaptive grid method for computing the equilibria of rotating self-gravitating barotropic gases

Mar 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...269..255g&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 269, no. 1-2, p. 255-266.

Statistics

Computation

2

Computational Grids, Cosmic Gases, Finite Difference Theory, Gravitational Effects, Rotating Fluids, Barotropic Flow, Equilibrium Flow, Stellar Evolution

Scientific paper

The paper describes a general iteration scheme, which appears to be the most effective in combination with finite-difference methods for the computation of equilibria of rotating self-gravitating gases. It presents an algorithm based on a combination of the iteration methods for the solution of the elliptic free boundary problem and the adaptive grids methods. The entire problem is formulated in the form of two elliptic equations for enthalpy and gravitational potential, respectively, and the Bernoulli integral is used as the boundary condition. As a result of simulations, the a priori unknown star's shape is calculated as well as a grid adapted to surfaces of constant pressure and pressure and gravitational potential distributions on that grid. In order to demonstrate the capabilities of the method a series of equilibrium sequences of differentially rotating polytropes with various adiabatic indices was computed.

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