Cocoon emission from Compact binary mergers (May 2017)

The picture to the left shows the logarithmic energy density of a 3D simulation, in which a hypermassive neutron star is collapsing, and as a result a jet is launched into the outflowing ejecta that comes from the double neutron star merger. The jet spends about a tenth of a second before it breaks out alongside the cocoon. We calculate numerically the cocoon cooling emission and its macronova.
Link to the paper

The EM counterpart of GW170817 (October 2017-March 2019)

The picture to the left shows a choked jet, which was injected into a hot expanding ejecta, but did not manage to break out of it. The jet energy is then deposited into the cocoon which continues to propagate inside the ejecta until breaking out of it. Upon breakout, energy is released in gamma-rays in two phases: planar and spherical. We show that this emission agrees very well with the observation of GRB170817A. Additionally this scenario fits to a very high degree with the UV/opt/IR and radio observations of this event.
Illuminating gravitational waves: A concordant picture of photons from a neutron star merger, Kasliwal et al.
The cocoon emission – an electromagnetic counterpart to gravitational waves from neutron star mergers, Gottlieb et al.
The γ -rays that accompanied GW170817 and the observational signature of a magnetic jet breaking out of NS merger ejecta, Bromberg et al.
A radio counterpart to a neutron star merger, Hallian et al.
A mildly relativistic wide-angle outflow in the neutron star merger GW170817, Mooley et al.
From γ to Radio - The Electromagnetic Counterpart of GW 170817, Nakar et al.
Superluminal motion of a relativistic jet in the neutron star merger GW170817, Mooley, Deller, Gottlieb et al.
Detectability of neutron star merger afterglows, Gottlieb et al.
Electromagnetic signals from the decay of free neutrons in the first hours of neutron star mergers, Gottlieb & Loeb