Speaker
Dr
Giovanni Camelio
(Stockholm University)
Description
An unstable rotating neutron star can collapse to a black hole.
A particle in the Innermost Stable Circular Orbit (ISCO) of this black hole has
the lowest possible angular momentum that prevents it to fall into the black hole.
Only the particles of the unstable neutron star that have a specific angular
momentum greater than that of the black hole ISCO will escape the collapse.
Using this criterion, we estimate the mass of the disk that might form in a
neutron star collapse for a variety of Equation Of States (EOSs).
This is achieved by analysing the neutron star equilibrium configurations obtained
with the XNS code and by checking our predictions with general relativistic
hydrodynamical simulations performed with the BAM code.
We find that for all considered EOSs the disk mass is too low to generate gamma
ray bursts with significant energy.
Primary author
Dr
Giovanni Camelio
(Stockholm University)
Co-authors
Prof.
Stephan Rosswog
(Stockholm University)
Dr
Tim Dietrich
(Nikhef, Amsterdam)
