{ "id": "1802.07732", "version": "v1", "published": "2018-02-21T19:00:02.000Z", "updated": "2018-02-21T19:00:02.000Z", "title": "Is the macronova in GW170817 powered by the central engine?", "authors": [ "Tatsuya Matsumoto", "Kunihito Ioka", "Shota Kisaka", "Ehud Nakar" ], "comment": "12 pages, 6 figures, submitted to ApJ, comments welcome!", "categories": [ "astro-ph.HE" ], "abstract": "The gravitational wave event GW170817 from a binary neutron star (NS) merger is accompanied by electromagnetic counterparts, and the optical and near-infared emission is called a macronova (or kilonova). Although the radioactivity of synthesized r-process elements is widely discussed as an energy source, its decisive evidence is not clearly shown yet. We discuss a macronova powered by the central engine activities such as jet activities and X-rays from the matter fallback, and show that the engine model allows much broader parameter spaces, in particular smaller ejecta mass ($\\sim10^{-4}-0.01\\,\\Msun$) than the r-process model. The blue and red macronovae are naturally explained by various combinations of the ejecta such as a cocoon and merger ejecta with the energy sources of jets and X-rays. The required energy injection is very similar to the X-ray excess observed in GRB 130603B with the power-law slope of $\\sim-1.3$. The required lanthanoid fraction for the opacity can be also consistent with the Galactic one. Early or late multi-wavelength observations are crucial for revealing the central engine of short gamma-ray bursts and the r-process nucleosynthesis.", "revisions": [ { "version": "v1", "updated": "2018-02-21T19:00:02.000Z" } ], "analyses": { "keywords": [ "gravitational wave event gw170817", "energy source", "short gamma-ray bursts", "binary neutron star", "broader parameter spaces" ], "note": { "typesetting": "TeX", "pages": 12, "language": "en", "license": "arXiv", "status": "editable" } } }