General Relativistic Decompression of Binary Neutron Stars During Dynamic Inspiral
Abstract
Description
We investigate the dynamic stability of inspiraling neutron stars by performing multiple-orbit numerical relativity simulations of the binary neutron star inspiral process. By introducing eccentricities in the orbits of the neutron stars, significant changes in orbital separation are obtained within orbital timescales. We find that as the binary system evolves from apastron to periastron (as the binary separation decreases), the central rest mass density of each star decreases, thus stabilizing the stars against individual prompt collapse. As the binary system evolves from periastron to apastron, the central rest mass density increases; the neutron stars re-compress as the binary separation increases.
Figure replaced, final published version. Dedicated to Rafael Sorkin on his 60th birthday
Figure replaced, final published version. Dedicated to Rafael Sorkin on his 60th birthday