TY - JOUR
T1 - Unequal mass binary neutron star mergers and multimessenger signals
AU - Lehner, Luis
AU - Liebling, Steven L.
AU - Palenzuela, Carlos
AU - Caballero, O. L.
AU - O'Connor, Evan
AU - Anderson, Matthew
AU - Neilsen, David
N1 - Funding Information:
This work was supported by the NSF under grants PHY-1308621(LIU), PHY-0969811 & PHY-1308727(BYU), NASAs ATP program through grant NNX13AH01G, NSERC through a Discovery Grant (to LL) and CIFAR (to LL). CP acknowledges support from the Spanish Ministry of Education and Science through a Ramon y Cajal grant and from the Spanish Ministry of Economy and Competitiveness grant FPA2013-41042-P. Additional support for this work was provided by NASA through Hubble Fellowship grant #51344.001-A (EO) awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. Research at Perimeter Institute is supported through Industry Canada and by the Province of Ontario through the Ministry of Research & Innovation. Computations were performed at XSEDE and Scinet.
Publisher Copyright:
© 2016 IOP Publishing Ltd.
PY - 2016/9/2
Y1 - 2016/9/2
N2 - 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.
AB - 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.
KW - binary neutron stars
KW - electromagnetic counterparts
KW - gravitational waves
KW - multimessenger astronomy
KW - numerical relativity
UR - http://www.scopus.com/inward/record.url?scp=84988521428&partnerID=8YFLogxK
U2 - 10.1088/0264-9381/33/18/184002
DO - 10.1088/0264-9381/33/18/184002
M3 - Article
AN - SCOPUS:84988521428
SN - 0264-9381
VL - 33
JO - Classical and Quantum Gravity
JF - Classical and Quantum Gravity
IS - 18
M1 - 184002
ER -