AAS Meeting #194 - Chicago, Illinois, May/June 1999
Session 29. White Dwarfs, Neutron Stars and Pulsars
Oral, Monday, May 31, 1999, 2:00-3:30pm, International Ballroom North

[Previous] | [Session 29] | [Next]

[29.03] Revised Relativistic Hydrodynamical Model for Neutron-Star Binaries

G. J. Mathews, C. Blakelock (U. Notre Dame), J. R. Wilson (LLNL and U. Notre Dame)

We report on the first numerical results from a corrected hydrodynamic simulation of binary neutron stars near merger. The new results show that for a given total angular momentum, the compression of neutron stars noted in previous simulations is still present although at a reduced level compared to the uncorrected results. However, at the same time, the inner most stable circular orbit moves to closer separation distances so that significant compression and even collapse to two black holes is still possible prior to merger. This reduced compression in the corrected simulation is consistent with other recent studies of irrotational binaries in quasiequilibrium in which the compression effect is observed to be small. Another significant effect of this correction is that the derived binary orbital frequencies are now in closer agreement with post-Newtonian expectations.

If the author provided an email address or URL for general inquiries, it is a s follows:


[Previous] | [Session 29] | [Next]