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Unequal mass binary neutron star mergers and multimessenger signals

Luis LehnerPerimeter Institute for Theoretical Physics, Waterloo, Ontario N2L 2Y5, CanadaSteven L LieblingDepartment of Physics, Long Island University, Brookville, NY 11548, USACarlos PalenzuelaDepartament de Física, Universitat de les Illes Balears and Institut d’Estudis Espacials e Catalunya, Palma de Mallorca, Baleares E-07122, SpainO L CaballeroDepartment of Physics, University of Guelph, Guelph, Ontario N1G 2W1, CanadaEvan O’ConnorDepartment of Physics, North Carolina State University, Raleigh, NC 27695, USAMatthew AndersonPervasive Technology Institute, Indiana University, Bloomington, IN 47405, USADavid NeilsenDepartment of Physics and Astronomy, Brigham Young University, Provo, UT 84602, USA

2016en

ABI

Annotatsiya

We study the merger of binary neutron stars with different mass ratios adopting three different realistic, microphysical nuclear equations of state, as well as incorporating neutrino cooling effects. In particular, we concentrate on the influence of the equation of state on the gravitational wave signature and also on its role, in combination with neutrino cooling, in determining the properties of the resulting hypermassive neutron star, of the neutrinos produced, and of the ejected material. The ejecta we find are consistent with other recent studies that find that small mass ratios produce more ejecta than equal mass cases (up to some limit) and this ejecta is more neutron rich. This trend indicates the importance with future kilonovae observations of measuring the individual masses of an associated binary neutron star system, presumably from concurrent gravitational wave observations, in order to be able to extract information about the nuclear equation of state

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DOI: 10.1088/0264-9381/33/18/184002

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