Instabilities in Close Neutron Star Binaries

Details Instabilities in Close Neutron Star Binaries Instabilities in Close Neutron Star Binaries

Dec 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995phrvl..75.4161w&link_type=abstract

Physical Review Letters, Volume 75, Issue 23, December 4, 1995, pp.4161-4164

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119

Spectroscopic Binaries, Close Binaries, Numerical Relativity, Relativistic Stars: Structure, Stability, And Oscillations, Neutron Stars

Scientific paper

We report on a new analysis of instabilities in close neutron star binaries based upon (3+1) dimensional general relativistic numerical hydrodynamics calculations. When a realistic equation of state is employed, orbit calculations for two 1.45Msolar neutron stars reveal surprising evidence that general relativistic effects may cause otherwise stable stars to individually collapse prior to merging. Also, the strong fields cause the last stable orbit to occur at a larger separation distance and lower frequency than post-Newtonian estimates.

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