Evolutionary sequences of irrotational binary neutron stars

摘要: We present results of numerical computations quasiequilibrium sequences binary neutron stars with zero vorticity, in the general relativistic framework. The Einstein equations are solved under assumption a conformally flat spatial 3-metric (Wilson-Mathews approximation). evolution central density each star is monitored as orbit shrinks response to gravitational wave emission. For compactification ratio M/R=0.14, remains rather constant (with slight increase, below 0.1%) before decreasing. higher M/R=0.17 (i.e. closer maximum mass configuration), very small increase (at most 0.3%) observed decrease. This effect within error induced by approximation. It can be thus concluded that no substantial compression found, which would have indicated tendency individually collapse black hole prior merger. Moreover, turning point has been found binding energy or angular momentum along evolutionary sequences, may indicate these systems do not any innermost stable circular (ISCO).