A versatile method for obtaining structures of rapidly rotating stars. II - Three-dimensional self-consistent field method

Details A versatile method for obtaining structures of rapidly rotating stars. II - Three-dimensional self-consistent field method A versatile method for obtaining structures of rapidly rotating stars. II - Three-dimensional self-consistent field method

Nov 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apjs...62..461h&link_type=abstract

Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 62, Nov. 1986, p. 461-499.

Statistics

Computation

81

Angular Velocity, Binary Stars, Computational Astrophysics, Self Consistent Fields, Stellar Rotation, Stellar Structure, Boundary Value Problems, Equations Of State, Four Body Problem, Stellar Mass, Three Body Problem, White Dwarf Stars

Scientific paper

A new three-dimensional computational method for obtaining structures of a rapidly rotating star and multiple star systems, including binaries, is formulated to calculate many kinds of structures, such as ellipsoids, dumbbells, and deep contact binaries. Four kinds of multibody systems including two-body binary, three-body, four-body, and five-body systems are computed; they are assumed to be rigidly rotating and composed of equal masses. For binary systems, the equilibrium sequences from ellipsoid to binary through dumbbell structure are computed for two kinds of equation of state: polytropic stars and zero-temperature white dwarfs. Three- and four-body systems become a three-lobed or a four-lobed configuration as the fluids come into contact, but a five-body system becomes a one-ring configuration finally. This implies that the five-body sequence bifurcates from the one-ring sequence, although two-, three-, and four-body sequences bifurcate from the spheroidal sequence.

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