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      Constraint on the ejecta mass for a black hole-neutron star merger event candidate S190814bv

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          Abstract

          We derive the upper limit to the ejecta mass of S190814bv, a black hole-neutron star merger candidate, through the radiative transfer simulations for kilonovae with the realistic ejecta density profile as well as the detailed opacity and heating rate models. The limits to the ejecta mass strongly depend on the viewing angle. For the face-on observations (\(\le45^\circ\)), the total ejecta mass should be smaller than \(0.1\,M_\odot\) for the average distance of S190814bv (\(D=267\) Mpc), while larger mass is allowed for the edge-on observations. We also derive the conservative upper limits of the dynamical ejecta mass to be \(0.02\,M_\odot\), \(0.03\,M_\odot\), and \(0.05\,M_\odot\) for the viewing angle \(\le 20^\circ\), \(\le 45^\circ\), and for \(\le 90^\circ\), respectively. We show that the iz-band observation deeper than \(22\) mag within \(2\) d after the GW trigger is crucial to detect the kilonova with the total ejecta mass of \(0.06\,M_\odot\) at the distance of \(D=300\) Mpc. We also show that a strong constraint on the NS mass-radius relation can be obtained if the future observations put the upper limit of \(0.03\,M_\odot\) to the dynamical ejecta mass for a BH-NS event with the chirp mass smaller than \(\lesssim 3\,M_\odot\) and effective spin larger than \(\gtrsim 0.5\).

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          Author and article information

          Journal
          05 February 2020
          Article
          2002.01662
          a72cb8db-44f5-444f-b44b-40da2c225463

          http://arxiv.org/licenses/nonexclusive-distrib/1.0/

          History
          Custom metadata
          16 pages, 15 figures. Submitted to ApJ
          astro-ph.HE gr-qc

          General relativity & Quantum cosmology,High energy astrophysical phenomena

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