http://arxiv.org/abs/2001.00205
It is believed that the relativistic jets of gamma-ray bursts (GRBs) should initially propagate through a heavy envelope of the massive progenitor stars or through a merger ejecta formed from the compact binary mergers. The interaction of a jet with a stellar envelope or a merger ejecta can lead to the deceleration of the head material of the jet and, simultaneously, the formation of a hot cocoon. However, this jet-envelope/ejecta interaction is actually undetectable with electromagnetic radiation and can only be inferred indirectly by the structure of the breakout jet. Therefore, as a way out of this difficulty, it is suggested that the jet-envelope/ejecta interaction can produce a gravitational wave memory of an amplitude of $h\sim10^{-27}-10^{-24}$, which could be detected with some future gravitational wave detectors sensitive in the frequency range of $f\sim 0.1-1$ Hz. This provides a potential direct way to probe the jet propagation and then the interior of the GRB progenitors. Moreover, this method is in principle available even if the jet is finally chocked in the stellar envelope or the merger ejecta.
Y. Yu
Fri, 3 Jan 20
33/45
Comments: 5 pages, 4 figures, Happy new year!