Physics
Scientific paper
Apr 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aps..aprh12001u&link_type=abstract
American Physical Society, APS April Meeting, April 14-17, 2007, abstract #H12.001
Physics
Scientific paper
Simulations for the merger of black hole-neutron star (BH-NS) binary are performed successfully in full general relativity, starting from the initial data in quasi-equilibrium circular orbit. A new method is developed for calculating the puncture BH-NS initial data in circular orbits. Then, the BH-NS binary is evolved using the moving puncture method. For the initial data, we assumed that the BH has no spin, while the NS has the corotating velocity field and follows the γ-law equations of state with γ=1. The BH mass is chosen to be MBH 3.2 M, and the NS mass to be MNS 1.4 M with relatively large radius ˜14km. It is found that the neutron star is tidally disrupted near the last orbit, ˜80% of the NS mass is swallowed into the BH, and the disk mass after the merger in this model is estimated as small as ˜0.3 M. The result indicates that the BH-disk system with the disk mass ˜M is not formed after the merger of non-spinning BH and NS binary, although a disk of mass ˜0.1 M is a possible outcome.
Shibata Masaru
Uryu Koji
No associations
LandOfFree
Simulations for the merger of black hole-neutron star binary in full general relativity. does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Simulations for the merger of black hole-neutron star binary in full general relativity., we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Simulations for the merger of black hole-neutron star binary in full general relativity. will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1684143