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 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. Papers: ► 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. 2018
The picture to the left shows the logarithmic energy density of a 3D simulation, in which a jet is launched from the core of a four solar mass star. The jet spends about two seconds in the star before it breaks out. Once it breaks out from the star, so does the cocoon, for which we calculate numerically the upcoming cooling emission. For cocoon's signature page
The picture to the left shows the four velocity of a 2D simulation, in which a jet is injected for one second before terminated and chocked. This system will therefore continues to evolve spherically. We calculate the upcoming emission, as all the jet energy is deposited in the cocoon, which will radiate it isotropically. For cocoon's signature page
The picture to the left shows the inertia and the four velocity of a 3D hydro jet. Instabilities emerge at the jet's spine soon after the first collimation shock, causing its disintegration. Two types of instablities are present: Rayleight Taylor instabilities in the plane perpendicular to the jet's axis, and Kelvin Helmholtz in the entire space, both operate at the shear between the jet's spine and the shocked jet around it.