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Issue A&A
Volume 376, Number 2, September II 2001
Page(s) 606 - 613
Section Formation, structure and evolution of stars
DOI http://dx.doi.org/10.1051/0004-6361:20011037



A&A 376, 606-613 (2001)
DOI: 10.1051/0004-6361:20011037

Velocity-induced collapses of stable neutron stars

J. Novak

Département d'Astrophysique Relativiste et de Cosmologie -UMR 8629 du CNRS, Observatoire de Paris, 92195 Meudon Cedex, France

(Received 22 May 2001 / Accepted 11 July 2001 )

Abstract
The collapse of spherical neutron stars is studied in General Relativity. The initial state is a stable neutron star to which an inward radial kinetic energy has been added through some velocity profile. For two different equations of state and two different shapes of velocity profiles, it is found that neutron stars can collapse to black holes for high enough inward velocities, provided that their masses are higher than some minimal value, depending on the equation of state. For a polytropic equation of state of the form $p=K\rho^\gamma $, with $\gamma = 2$ it is found to be $1.16 \left( \frac{K}{0.1} \right)^{0.5} M_{\odot}$, whereas for a more realistic one (described in Pons et al. 2000), it is $0.36 M_{\odot} $. In some cases of collapse forming a black hole, part of the matter composing the initial neutron star can be ejected through a shock, leaving only a fraction of the initial mass to form a black hole. Therefore, black holes of very small masses can be formed and, in particular, the mass scaling relation, as a function of initial velocity, takes the form discovered by Choptuik (1993) for critical collapses.


Key words: stars: neutron -- black hole physics -- hydrodynamics -- relativity

SIMBAD Objects in preparation



© ESO 2001

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