Equilibrium models of differentially rotating, completely catalyzed, zero-temperature configurations with central densities intermediate to white dwarf and neutron star densities

Details Equilibrium models of differentially rotating, completely catalyzed, zero-temperature configurations with central densities intermediate to white dwarf and neutron star densities Equilibrium models of differentially rotating, completely catalyzed, zero-temperature configurations with central densities intermediate to white dwarf and neutron star densities

Nov 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...152..325m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 152, no. 2, Nov. 1985, p. 325-335.

Astronomy and Astrophysics

Astrophysics

22

Neutron Stars, Stellar Evolution, Stellar Models, Stellar Structure, White Dwarf Stars, Angular Momentum, Density Distribution, Polytropic Processes, Stellar Mass, Stellar Rotation, Supernovae

Scientific paper

We have calculated axisymmetric equilibria of differentially rotating, completely catalyzed, zero-temperature Newtonian configurations with central densities in the range 10 7 gcm-3 <= Qc < 5 1014 gcm -3. Our aim was to address the following question: is it possible for rotating white dwarfs with a mass larger than the Chandrasekhar mass to evolve, via angular momentum losses, to a neutron star on a secular time scale, i.e. without a sudden release of gravitational energy in the form of an optical supernova outburst? Our results show that dynamically stable (against collapse) rotating equilibrium models exist up to densities of ≍ 1011 gcm-3 (without rotation ≍ 10 9 gcm-3) and with masses up to 1.7 Msun (without rotation 1.0 Msun). Configurations with masses in the range 1.7 < M/Msun < 2.2 are also dynamically stable, but secularly unstable against non-axisymmetric perturbations. We find that for all studied combinations of mass, angular momentum and angular momentum distribution the evolution of a rotating (cold) white dwarf must become dynamic at densities around 1012 gcm-3, i.e. roughly 80 % of the neutron star's binding energy will be released on a dynamical time scale.

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