Internal temperature of isothermal neutron star core matter

Details Internal temperature of isothermal neutron star core matter Internal temperature of isothermal neutron star core matter

Mar 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989ap%26ss.153...55f&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 153, no. 1, March 1989, p. 55-60. Research supported by the Council of Sci

Statistics

Computation

Computational Astrophysics, Neutron Stars, Nuclear Astrophysics, Stellar Interiors, Stellar Temperature, Equations Of State, Stellar Envelopes, Stellar Evolution

Scientific paper

Two new equations of state were obtained from the relativistic thermodynamics relation for isothermal degenerate neutron-star (NS) cores and from the isentropic nature of matter in the NS, by assuming the equalities Gamma = Gamma(2) and Gamma = Gamma(3) (where Gammas are usual adiabatic exponents), respectively. These new equations were used to derive the internal temperature of the NS core. The temperature of the nuclear matter was obtained as T = Ta(P + E)/rho, where P is pressure, E is energy density, and rho is rest mass density. Variation of T/Ta with energy density for different central conditions was determined. It was found that the variations of T/Ta with log E(0) were linear and were almost identical for these conditions.

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