Maximum mass instability of neutron stars and weak interaction processes in dense matter

Details Maximum mass instability of neutron stars and weak interaction processes in dense matter Maximum mass instability of neutron stars and weak interaction processes in dense matter

Feb 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...294..747g&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 294, no. 3, p. 747-756

Astronomy and Astrophysics

Astrophysics

15

Neutron Stars, Stability, Stellar Mass, Stellar Models, Weak Interactions (Field Theory), Hydrodynamics, Linear Equations, Perturbation Theory, Thermodynamic Equilibrium

Scientific paper

We study the stability of equilibrium configurations of neutron stars in the vicinity of maximum allowable mass (mass M approximately equals Mmax, central density rhoc approximately equals rhoc, max. The effect of weak interaction processes on the dynamical properties of perturbed stars is studied. Linear analysis performed for a specific model of dense matter shows, that due to the slowness of weak interaction processes, the region of configurations stable with respect to infinitesimal radial perturbations extends beyond rhoc, max. Finite amplitude analysis of stability is performed using fully relativistic spherically symmetric hydrodynamical code. We show that for rhoc close to rhoc, max, configurations with rhoc less than rhoc, max can become unstable with respect to a finite amplitude perturbation. Similarly, those configurations with rhoc greater than rhoc, max, which were stable in the linear regime, can be destabilized, due to non-linear effects, by a small but finite amplitude perturbation which exceeds some threshold value. In all cases, destabilized metastable configurations collapse into a black hole.

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