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2.5 Going further

The AIC scenario is generally discussed in terms of the collapse of an accreting white dwarf to a neutron star. However, Shibata, Baumgarte, and Shapiro have examined the collapse of a rotating, supramassive neutron star to a black hole [224]. Such supramassive neutron stars (with masses greater than the maximum mass for a nonrotating neutron star) could be formed and pushed to collapse via accretion from a binary companion. They performed 3D, fully general relativistic hydrodynamics simulations of uniformly rotating neutron stars. Dynamical non-axisymmetric instabilities (such as the bar-mode) did not have time to grow in their simulations prior to black hole formation. Differentially rotating neutron star progenitors could have higher values of b than the uniformly rotating models used in this study and may be susceptible to non-axisymmetric instabilities on a shorter timescale.


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