Speaker
Tsvi Piran
Description
It is widely accepted that short GRBs are associated from
neutron star mergers. As
these mergers involve a significant mass ejection, the GRB
jet must penetrate this
mass before producing the observed radiation. As the jet
propagates within the ejecta
is create a hot cocoon containing a significant amount of
energy. Eventually the
cocoon breakout from the ejecta and produces a bright
optical/uv signal lasting a few
hours. A rapid followup of a gravitational radiation signal
might enable us to detect
this signal and identify the location of the merger.
