TY - JOUR
T1 - Neutron Star Equation of State in Light of GW190814
AU - Tan, Hung
AU - Noronha-Hostler, Jacquelyn
AU - Yunes, Nico
N1 - Funding Information:
The authors would like to thank Veronica Dexheimer, Hank Lamm, and Mauricio Hippert for useful discussions related to this work. J. N. H. acknowledges the support of the Alfred P. Sloan Foundation, and support from the US-DOE Nuclear Science Grant No. DE-SC0019175. H. T. and N. Y. acknowledge support from NASA Grants No. NNX16AB98G, No. 80NSSC17M0041, and No. 80NSSC18K1352 and NSF Grant No. 1759615. The authors also acknowledge support from the Illinois Campus Cluster, a computing resource that is operated by the Illinois Campus Cluster Program (ICCP) in conjunction with the National Center for Supercomputing Applications (NCSA), and which is supported by funds from the University of Illinois at Urbana-Champaign.
Publisher Copyright:
© 2020 American Physical Society.
PY - 2020/12/30
Y1 - 2020/12/30
N2 - The observation of gravitational waves from an asymmetric binary opens the possibility for heavy neutron stars, but these pose challenges to models of the neutron star equation of state. We construct heavy neutron stars by introducing nontrivial structure in the speed of sound sourced by deconfined QCD matter, which cannot be well recovered by spectral representations. Their moment of inertia, Love number, and quadrupole moment are very small, so a tenfold increase in sensitivity may be needed to test this possibility with gravitational waves, which is feasible with third generation detectors.
AB - The observation of gravitational waves from an asymmetric binary opens the possibility for heavy neutron stars, but these pose challenges to models of the neutron star equation of state. We construct heavy neutron stars by introducing nontrivial structure in the speed of sound sourced by deconfined QCD matter, which cannot be well recovered by spectral representations. Their moment of inertia, Love number, and quadrupole moment are very small, so a tenfold increase in sensitivity may be needed to test this possibility with gravitational waves, which is feasible with third generation detectors.
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U2 - 10.1103/PhysRevLett.125.261104
DO - 10.1103/PhysRevLett.125.261104
M3 - Article
C2 - 33449737
AN - SCOPUS:85099167027
SN - 0031-9007
VL - 125
JO - Physical review letters
JF - Physical review letters
IS - 26
M1 - 261104
ER -