Bivariate numerical models for a rotating, pion-condensed neutron star

Details Bivariate numerical models for a rotating, pion-condensed neutron star Bivariate numerical models for a rotating, pion-condensed neutron star

Jun 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986pazh...12..383b&link_type=abstract

(Pis'ma v Astronomicheskii Zhurnal, vol. 12, May 1986, p. 383-387) Soviet Astronomy Letters (ISSN 0360-0327), vol. 12, May-June

Astronomy and Astrophysics

Astronomy

Bivariate Analysis, Neutron Stars, Pions, Stellar Gravitation, Stellar Rotation, Density Distribution, Equations Of State, Iterative Solution, Stellar Envelopes, Stellar Mass Ejection, Time Marching

Scientific paper

The paper presents numerical solutions to axisymmetric gravitational gas-dynamics equations for neutron stars with a nonmonotonic equation of state. It is shown that the development of the pion-condensate phase transition will trigger an outward shock and produce a rotational-velocity discontinuity at the density interface. It is noted that only a thin envelope layer will be ejected.

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