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Open AccessArticle

Identifying Quark Matter in Hybrid Stars through Relativistic Tidal Deformations

1
Department of Physics & Astronomy, California State University Long Beach, Long Beach, CA 90840, USA
2
Department of Physics, Stanford University, Stanford, CA 94305, USA
3
College of Science, Huazhong Agricultural University, Wuhan 430070, China
*
Author to whom correspondence should be addressed.
Universe 2019, 5(9), 193; https://doi.org/10.3390/universe5090193
Received: 9 May 2019 / Revised: 19 August 2019 / Accepted: 23 August 2019 / Published: 30 August 2019
We study a specific model of neutron star matter that supports a phase transition to quark matter at high density and examine parameter ranges for consistency with the mass-weighted tidal deformability of Λ ˜ = 300 230 + 420 for a mass ratio of q [ 0.73 , 1.0 ] , as inferred from observations of gravitational waves from the binary neutron star merger event GW170817. By using this observation to restrict the parameter space for the equation of state (EoS) model used throughout this study, we aim to assess the possibility of a potential solution to the masquerade and flavor camouflage problems for hybrid EoS models. Assuming the two stars have the same EoS, in which the Dirac-Brueckner-Hartree Fock (DBHF) nuclear model transitions to the vBag quark model, we see if the parameter space of these hybrid model stars are restricted due to the adherence to the reported Λ 1.4 70 , 580 and M m a x [ 2.01 , 2.16 ] M constraints. Upon completion, we find that, while the parameter space for our model does get restricted, it does not ultimately resolve the masquerade and flavor camouflage problems. View Full-Text
Keywords: compact stars; mixed phases; gravitational waves; equation of state; tidal deformability; QCD; quark–hadron phase transitions compact stars; mixed phases; gravitational waves; equation of state; tidal deformability; QCD; quark–hadron phase transitions
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Irving, B.; Klähn, T.; Jaikumar, P.; Salinas, M.; Wei, W. Identifying Quark Matter in Hybrid Stars through Relativistic Tidal Deformations. Universe 2019, 5, 193.

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