![]() ![]() 2017b), was accompanied by a short GRB (Abbott et al. The first detection of a binary neutron star merger, GW170817 (Abbott et al. ![]() The data release from the third observing run brought the total number of confidently detected binary BH coalescences to approximately 70 (Abbott et al. Since then, nine more binary BH coalescences were observed during the first and second observing runs of advanced LIGO and Virgo detectors (Abbott et al. 2015) detected the first chirp of gravitational waves from a binary BH merger, GW150914 (Abbott et al. On 14 September, 2015, the advanced Laser Interferometer Gravitational-wave Observatory (LIGO, Aasi et al. The intervening decade has completely changed this landscape. Therefore, most of the rate predictions, particularly for mergers involving black holes (BHs), were based purely on theoretical models (see, e.g., Mandel and O’Shaughnessy 2010 for a review of the status of models at that time). But no actual compact object mergers were definitively observed. It was believed that short gamma-ray bursts (SGRBs) were associated with mergers of two NSs. At that time, a handful of ultimately merging double neutron star (NS) systems in the Milky Way Galaxy were known from radio pulsar observations, starting with the discovery of Hulse and Taylor ( 1975). It has been more than a decade since Abadie ( 2010) reviewed the literature on compact-object merger rate predictions. ![]()
0 Comments
Leave a Reply. |