Since 2005, which was the break-through year in the field of numerical relativity, the
simulation of binaries composed of BHs has been feasible. Soon after the first success for
the simulation of BH-BH binaries [162], work on the merger of BH-NS binaries was
published [202
, 203
, 197
, 62
, 58
, 63
, 194
, 57
, 107
, 108
, 41
, 74
, 154
, 109
]. Shibata and his
collaborators (hereafter the Kyoto/Tokyo (KT) group) performed a fully general relativistic
simulation for a BH-NS binary merger for the first time, extending their earlier works for NS-NS
binaries [193, 200, 201, 198, 199
, 196]. Soon after the success of the KT group, the University of Illinois
at Urbana-Champaign (UIUC) and Caltech/Cornell/CITA/Washington State University (CCCW)
groups also performed simulations for BH-NS binary merger. The UIUC group extended their
earlier work on NS-NS binaries [59], and the CCCW group extended their work for BH-BH
binaries [30
, 31
, 181
] incorporating the hydrodynamics equation solvers [57
]. Subsequently, several
scientific results have been derived recently by these groups. In addition, in 2010, the Louisiana State
University/Brigham Young University/Perimeter Institute/Long Island University/Indiana
University (LBPLI) and Albert Einstein Institute (AEI) groups published their first results for the
BH-NS binary merger [41
, 154
]. All these groups will report with more sophisticated physics
incorporating nuclear-theory-based EOS, microphysical processes, and magnetic-field effects in the
near future. Thus, in the following sections, we focus only on reviewing the current status of
the general relativistic studies (see also [56] for a review of the latest status of this field in
2010).
http://www.livingreviews.org/lrr-2011-6 |
Living Rev. Relativity 14, (2011), 6
![]() This work is licensed under a Creative Commons License. E-mail us: |