Volume 376, Number 2, September II 2001
|Page(s)||606 - 613|
|Section||Interstellar and circumstellar matter|
|Published online||15 September 2001|
Velocity-induced collapses of stable neutron stars
Département d'Astrophysique Relativiste et de Cosmologie -UMR 8629 du CNRS, Observatoire de Paris, 92195 Meudon Cedex, France
Accepted: 11 July 2001
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 , with it is found to be , whereas for a more realistic one (described in Pons et al. [CITE]), it is . 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 ([CITE]) for critical collapses.
Key words: stars: neutron / black hole physics / hydrodynamics / relativity
© ESO, 2001
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.