Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...290..674a&link_type=abstract
Astronomy and Astrophysics 290, 674-681 (1994)
Astronomy and Astrophysics
Astrophysics
8
Numerical Methods, Stars: Interiors, Stars: Rotation
Scientific paper
A new computational method for the construction of rapidly rotating stellar models is described; it combines the high (quadratic) convergence of the Newton-Raphson procedure with the use of a fine mesh, typical of self-consistent field schemes. For the presentation of the gravitational potential a finite difference approximation to the Poisson equation is used, and the iterations of the potential are used to find the distribution of matter consistent with its gravity. It is necessary to solve a huge system of linear equations on every iteration step, but the matrix of the system is sparse, so that powerful sparse matrix solvers can be applied here. The high convergence rate of the iteration procedure and a robust sparse system solver warrant the high accuracy of calculations. The method is powerful enough for the description of models with a large density contrast and high T/|W|, where T and W are total kinetic and gravitational energy respectively. The efficiency of the method is tested in calculations of the stationary states for polytropes for T/|W| up to 0.425.
Aksenov Alexey G.
Blinnikov Sergei I.
No associations
LandOfFree
A Newton iteration method for obtaining equilibria of rapidly rotating stars does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with A Newton iteration method for obtaining equilibria of rapidly rotating stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and A Newton iteration method for obtaining equilibria of rapidly rotating stars will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1067522