Other
Scientific paper
Feb 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985ap%26ss.109..241d&link_type=abstract
Astrophysics and Space Science (ISSN 0004-640X), vol. 109, no. 2, Feb. 1985, p. 241-248.
Other
4
Neutron Stars, Stellar Cores, Stellar Structure, Equations Of State, Isothermal Processes, Relativistic Effects, Stellar Envelopes, Stellar Mass, Stellar Oscillations
Scientific paper
The authors have shown that some of the standard equations of state, when applied to NS cores, correspond to constancy of some adiabatic exponents. It has been shown that the equation of state, P = KE, corresponds to Γ1 = Γ2 = Γ3 = 1+K and the equation of state, dP/dE = K, corresponds to Γ3 = 1+K. For isothermal NS, the local temperature T can be expressed in terms of pressure P, energy density E, and rest mass density ρ. Equation of state corresponding to Γ = Γ2 is obtained as: P = E/ln(K/E) and the equation corresponding to Γ = Γ3 comes out as: E = P ln(K/P). When core equation corresponding to Γ = Γ2 or Γ = Γ3 is used in the core, the continuity of dP/dE at the core-envelope boundary can be ensured, along with the continuity of P, E, λ, and ν. The parameters of isothermal NS cores corresponding to the cases Γ = Γ2 and Γ = Γ3, have been obtained. The maximum mass of these NS cores comes out to be 2.7M_sun;.
Durgapal M. C.
Fuloria R. S.
Pande Kanchan
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