Simple equations for general relativistic hydrodynamics in spherical symmetry applied to neutron star collapse

Details Simple equations for general relativistic hydrodynamics in spherical symmetry applied to neutron star collapse Simple equations for general relativistic hydrodynamics in spherical symmetry applied to neutron star collapse

Dec 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...252..651g&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 252, no. 2, Dec. 1991, p. 651-663.

Astronomy and Astrophysics

Astronomy

34

Black Holes (Astronomy), Gravitational Collapse, Neutron Stars, Relativity, Baryons, Equations Of State, Euler Equations Of Motion, Hydrodynamic Equations, Stellar Oscillations

Scientific paper

A complete system of simple equations for general relativistic (GR) Eulerian hydrodynamics in spherical symmetry is presented, with variables different from those commonly used. In particular, a 'physical' fluid-velocity field (instead of a momentum density) is introduced, for which a GR generalization of the Euler equation is derived. The other dynamical equations are found to be in a perfect Newtonian form. As an application, the problem of stability and collapse of a neutron star near the maximum mass is investigated with a hydrodynamical code based on spectral methods. The latter integrates forward in time the whole system of equations starting with an hydrostatic equilibrium model built upon a realistic equation of state. Depending whether the equilibrium is theoretically stable or unstable, small radial oscillations or catastrophic collapse are observed. As the central density increases, the development of the instability is shown to be due to the growth of the fundamental mode of the oscillations. When the star becomes unstable, the collapse is followed up to the formation of a black hole.

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