The boundary conditions for relativistic polytropic fluid spheres

Details The boundary conditions for relativistic polytropic fluid spheres The boundary conditions for relativistic polytropic fluid spheres

Mar 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993ap%26ss.201..249d&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 201, no. 2, p. 249-271.

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Boundary Conditions, Polytropic Processes, Relativistic Effects, Spheres, Computational Astrophysics, Differential Equations, Numerical Integration

Scientific paper

The boundary conditions for relativistic polytropic fluid spheres are determined by solving the differential equations governing relativistic polytropic fluid spheres, using a variable-order Adams-Bashford-Moulton method (Samping and Gordon, 1975) modified to work in the complex plane. The roots were found using the classical Secant method, using the real part of the complex numbers provided by the integrating algorithm. The numerical method was checked for sigma = 0 against accurate boundary conditions for classical polytropes (Jabbar, 1984). The results are in agreement within 7 to 10 digits for n less than 4; for n larger than 4, the accuracy declines to a minimum of 5 digits for n larger than 4.5.

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