Phase transitions in stellar cores. I - Equilibrium configurations

Details Phase transitions in stellar cores. I - Equilibrium configurations Phase transitions in stellar cores. I - Equilibrium configurations

Sep 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...126..121s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 126, no. 1, Sept. 1983, p. 121-145. Sponsorship: U.S. - Maria Skolodowska-Curi

Astronomy and Astrophysics

Astrophysics

10

Neutron Stars, Phase Transformations, Stellar Cores, Stellar Models, White Dwarf Stars, Gravitation Theory, Incompressible Fluids, Mathematical Models, Moments Of Inertia, Polytropic Processes, Radii, Stellar Mass

Scientific paper

The effect of a first order phase transition occurring in the central core of a degenerate star is investigated based on the Newtonian theory of gravitation. Expressions for the changes of parameters such as the radius, the moment of inertia, or the energy during the transition from a one-phase to a two-phase star are given by means of analytical formulas that are valid for any equation of state. These formulas are shown to rely on the linearization of the equations of hydrostatic equilibrium supplemented by some suitable nonlinear corrections, and they are found to be accurate even for moderately large changes of the stellar parameters. The stability of the two-phase stars with respect to small radial perturbations is examined, and the properties of polytropic condensed cores are determined. It is shown that cores with an adiabatic index less than 4/3 can exist and be stable, but their mass, radius, and central densities must be smaller than some given values that are calculated. It is concluded that the study of the nondegenerate case, as well as the general relativistic case and also the time-dependent case, is a rather direct generalization of the theory, with a similar degree of accuracy.

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