Core-envelope models for massive fluid spheres

Details Core-envelope models for massive fluid spheres Core-envelope models for massive fluid spheres

Jan 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989ap%26ss.151..255f&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 151, no. 2, Jan. 1989, p. 255-264. Research supported by the Council of Sc

Astronomy and Astrophysics

Astrophysics

Neutron Stars, Stellar Cores, Stellar Envelopes, Stellar Models, Equations Of State, Rotating Fluids, Stellar Rotation

Scientific paper

The solution of the equation of state corresponding to the equality Gamma = Gamma3 gives nonterminating solutions for isothermal neutron star cores. Hence, for this equality, core-envelope models have been developed by taking another equation of state, corresponding to the condition Gamma3 = constant, in the envelope. Various static, pulsational, and rotational parameters pertaining to neutron star models are calculated. These models are gravitationally bound and stable for radial perturbations and slow rotations.

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