{ "id": "1705.10797", "version": "v1", "published": "2017-05-30T18:00:02.000Z", "updated": "2017-05-30T18:00:02.000Z", "title": "The cocoon emission - an electromagnetic counterpart to gravitational waves from neutron star mergers", "authors": [ "Ore Gottlieb", "Ehud Nakar", "Tsvi Piran" ], "categories": [ "astro-ph.HE" ], "abstract": "Short Gamma-Ray Bursts (SGRBs) are believed to arise from compact binary mergers (either neutron star-neutron star or black hole-neutron star). If so their jets must penetrate outflows that are ejected during the merger. As a jet crosses the ejecta it dissipates its energy, producing a hot cocoon which surrounds it. We present here 3D numerical simulations of jet propagation in mergers' outflows and we calculate the resulting emission. This emission consists of two components: the cooling emission, the leakage of the thermal energy of the hot cocoon, and the cocoon macronova that arises from the radioactive decay of the cocoon's material. This emission gives a brief (~ one hour) blue, wide angle signal. While the parameters of the outflow and jet are uncertain, for the configurations we have considered the signal is bright (~ -14 $-$ -15 absolute magnitude) and outshines all other predicted UV-optical signals. The signal is brighter when the jet breakout time is longer and its peak brightness does not depend strongly on the highly uncertain opacity. A rapid search for such a signal is a promising strategy to detect an electromagnetic merger counterpart. A detected candidate could be then followed by deep IR searches for the longer but weaker macronova arising from the rest of the ejecta.", "revisions": [ { "version": "v1", "updated": "2017-05-30T18:00:02.000Z" } ], "analyses": { "keywords": [ "neutron star mergers", "cocoon emission", "gravitational waves", "electromagnetic counterpart", "hot cocoon" ], "note": { "typesetting": "TeX", "pages": 0, "language": "en", "license": "arXiv", "status": "editable" } } }