Unequal mass binary neutron star mergers and multimessenger signals

By Luis Lehner, Steven L. Liebling, Carlos Palenzuela, O. L. Caballero, E. O’Connor, Matthew Anderson, D. Neilsen. 2016

134 citations recorded by the source corpus.

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.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/49902ba531fe092e234f5d578e1ff7718a09b5bf

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Citations in the corpus

Binary Neutron Star Mergers: Mass Ejection, Electromagnetic Counterparts, and Nucleosynthesis (2018, methodology): “…with a microphysical treatment of NS matter and with different levels of approximation for neutrino-radiation effects have also become available (Sekiguchi et al. 2011, 2015, 2016; Palenzuela et al. 2015; Foucart et al. 2016b; Lehner et al. 2016; Radice et al. 2016b; Bovard et al. 2017).”
Impact of ejecta morphology and composition on the electromagnetic signatures of neutron star mergers (2017, background): “Numerical simulations indicate that this type of outflow has velocities in the subrelativistic regime ∼ 0.1 − 0.3 c, is very neutron-rich (Ye ∼ 0.03 − 0.2), and has masses in the range ∼ 10−4 − 0.05 M (Rosswog 2013; Bauswein et al. 2013; Hotokezaka et al. 2013; Sekiguchi et al. 2016; Lehner et al. 2”
Constraints on the neutron star equation of state from AT2017gfo using radiative transfer simulations (2018, background): “…compact binary, the compact object masses, spins, orbital eccentricity, as well as the properties of NSs, such as the EOS (Rosswog et al. 1999; Bauswein et al. 2013b; Hotokezaka et al. 2013; Lehner et al. 2016; Radice et al. 2016; Dietrich & Ujevic 2017; Abbott et al. 2017f; Siegel & Metzger 2017).”
GW170817: Joint Constraint on the Neutron Star Equation of State from Multimessenger Observations (2017, background): “01~ of material can be unbound dynamically during the merger itself (Bauswein et al. 2013b; Hotokezaka et al. 2013; Lehner et al. 2016; Radice et al. 2016; Sekiguchi et al. 2016; Bovard et al. 2017; Dietrich et al. 2017b), although larger ejecta masses can be reached for small mass ratios q 0.6…”
Formation of Double Neutron Star Systems (2017, background): “…produce rprocess rich ejecta with larger asymmetry and a different direction-dependent composition than those expected for a DNS merger with q ≃ 1 (Just et al. 2015); and possibly, but not necessarily, a larger yield (depending on the NS masses and the NS EoS, Just et al. 2015; Lehner et al. 2016).”