Speaker
Dr
Gergely Debreczeni
(Wigner RCP)
Description
Modern gravitational wave (GW) detectors are hunting for GWs originating from various sources among other from binary neutron star (BNS) coalescence. It is assumed that in some cases it is the coalescence (merging) of such BNS system which is responsible for the creation of gamma-ray bursts (GRBs) - routinely detected by electromagnetic observatories. Since already well before their merging, during the inspiral phase, the binary system emits GWs, analysis groups of GW detectors are performing in-depth search for such events around the time-window of known, already detected GRBs. These joint analysis are very important in increasing the confidence of a possible GW detection.
It is widely expected that the first direct detection of GWs will happen in the next few years, and what is a matter of fact that the sensitivity of the next generation of GW detectors will allow us to 'see' a few hundred seconds of inspiral of the binary system before the merge - for specific mass parameter range.
From the two above fact, it naturally follows, that one can (should!) turn around the logic and use the GWs emitted during the inspiral phase of a BNS coalescence process to predict, in advance the time and sky location of a GRB and set up constraints on the physical parameters of the system. There exists no such prediction algorithm, as of today.
Despite the fact that it is not yet feasible to use this new method with the current GW detectors, it will be of utmost importance in the late-Advanced LIGO/Virgo era and definitely for Einstein Telescope.
The very goal of the research presented in this talk is to develop the above described zero-latency, BNS coalescence 'forecasting' method and set up and organize the associated alert system to be used by next generation of gravitational wave detectors and collaborating EM observatories.
Primary author
Dr
Gergely Debreczeni
(Wigner RCP)
