Polytropic equilibrium figures of equal mass

Details Polytropic equilibrium figures of equal mass Polytropic equilibrium figures of equal mass

Nov 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984ap%26ss.106..151m&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 106, no. 1, Nov. 1984, p. 151-160.

Statistics

Computation

Computational Astrophysics, Equilibrium Equations, Polytropic Processes, Stellar Mass, Stellar Models, Stellar Structure, Boundary Conditions, Boundary Value Problems, Elliptic Differential Equations, Newton-Raphson Method, Potential Theory

Scientific paper

A numerical computation technique for the solution of polytropic equilibrium figures for astrophysical potential problems such as degenerate-star models is developed and demonstrated. The technique is a modification of the semidiscrete pseudospectral method of Miketinac and Parter (1981) and employs a Newton-Raphson procedure combined with two different discretization schemes to solve the free boundary problem for a mildly nonlinear elliptic partial differential equation. The boundary conditions are set to make the mass of all computed figures equal and constant, and the global matrix of the discrete problem is manipulated to be symmetric. Numerical results for the sequence of figures of the polytrope with n = 1.5 are presented graphically and shown to be in good agreement with those obtained by Stoeckly (1965) using an indirect method.

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