Signals in the tidal deformability for phase transitions in compact stars with constraints from GW170817

Christian, Jan-Erik; Zacchi, Andreas; Schaffner-Bielich, J.

doi:10.1103/physrevd.99.023009

Cited by 100 publications

(109 citation statements)

References 53 publications

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“…6 (b). Furthermore, an additional H-Q2 curve lies below the diagonal, which implies that for M 1 M 2 one has Λ 1 Λ 2 , which is contrary to the expectation that Λ 1 Λ 2 , as already observed by several authors [11][12][13][14][15].…”

Section: Comparison With the Data From Gw170817 Eventmentioning

confidence: 60%

“…One possibility is a deconfinement phase transition from bound hadronic states to liberated quark states. The effect of a strong first-order phase transition on tidal deformabilities of the neutron star in the context of GW170817 event has been explored by a number of * jiajieli@itp.uni-frankfurt.de † sedrakian@fias.uni-frankfurt.de ‡ alford@physics.wustl.edu groups [5][6][7][8][9][10][11][12][13][14][15] showing that the hadron-quark phase transition at low enough density, ρ 2-3ρ 0 , where ρ 0 is the nuclear saturation density, relaxes the tension between the inferred tidal deformabilities and those predicted by purely hadronic models without a phase transition. Of particular interest in this context is the emergence of twin stars, where purely nucleonic and hybrid stars have the same masses, but different radii [6].…”

Section: Introductionmentioning

confidence: 99%

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Relativistic hybrid stars with sequential first-order phase transitions and heavy-baryon envelopes

Sedrakian

Alford

2020

Phys. Rev. D

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We compute the mass, radius and tidal deformability of stars containing phase transitions from hadronic to quark phase(s). These quantities are computed for three types of hadronic envelopes: purely nuclear, hyperonic, and ∆-resonance-hyperon admixed matter. We consider either a single first-order phase transition to a quark phase with a maximally stiff equation of state (EoS) or two sequential first-order phase transitions mimicking a transition from hadronic (H) to a quark matter phase followed by a second phase transition to another quark phase. Such a construct emulates the results of the computations of the EoS which include 2SC and CFL color superconducting phases at low and high density. We explore the parameter space which produces low mass twin and triplet configurations where equal mass stars have substantially different radii and tidal deformabilities. We demonstrate that while for purely hadronic stiff EoS the obtained maximum mass is inconsistent with the upper limit on this quantity placed by GW170817, the inclusion of the hyperonic and ∆-resonance degrees of freedom, as well as the deconfinement phase transition at sufficiently low density, produce configuration of stars consistent with this limit. The obtained hybrid star configurations are in the mass range relevant for the interpretation of the GW170817 event. We compare our results for the tidal deformability with the limits inferred from GW170817 showing that the onset of non-nucleonic phases, such as ∆-resonance-hyperon admixed phase or/and the quark phase(s) is favored by this data if the nuclear EoS is stiff. Also, we show that low-mass twins and especially triplets proliferate the number of combinations of possible types of star that can undergo a merger event, the maximal number being six in the case of triplets. The prospects for uncovering the first-order phase transition(s) to and in quark matter via measurements of tidal deformabilities in merger events are discussed.

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Section: Comparison With the Data From Gw170817 Eventmentioning

confidence: 60%

Section: Introductionmentioning

confidence: 99%

Relativistic hybrid stars with sequential first-order phase transitions and heavy-baryon envelopes

Sedrakian

Alford

2020

Phys. Rev. D

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“…Depending on the features of the phase transition of the hybrid star, twin-star solutions and the two branches in M (R) might appear. Indeed, information from gravitational waves is being exploited to better understand the twin-star scenario [217,189,219,220,222].…”

Section: Twin Starsmentioning

confidence: 99%

“…The maximum masses in the two branches allow a simple classification to order the discussion The tidal deformability also displays two distinct branches having the same mass [217,222], an additional smoking gun signature for the existence of twin stars.…”

Section: Twin Starsmentioning

confidence: 99%

Hadron matter in neutron stars in view of gravitational wave observations

Llanes-Estrada

Lope-Oter

2019

Progress in Particle and Nuclear Physics

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In this review we highlight a few physical properties of neutron stars and their theoretical treatment inasmuch as they can be useful for nuclear and particle physicists concerned with matter at finite density (and newly, temperature). Conversely, we lay out some of the hadron physics necessary to test General Relativity with binary mergers including at least one neutron star, in view of the event GW170817: neutron stars and their mergers reach the highest matter densities known, offering access to the matter side of Einstein's equations. In addition to minimum introductory material for those interested in starting research in the field of neutron stars, we dedicate quite some effort to a discussion of the Equation of State of hadron matter in view of gravitational wave developments; we address phase transitions and how the new data may help; we show why transport is expected to be dominated by turbulence instead of diffusion through most if not all of the star, in view of the transport coefficients that have been calculated from microscopic hadron physics; and we relate many of the interesting physics topics in neutron stars to the radius and tidal deformability.

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“…Effects on this quantity related to the appearance of quark matter in the inner cores of compact stars have been studied in Refs. [9,10]. Analysis of the data also serve to constraint the chirp mass of system, which determines (to leading-order) the evolution of binary NSs orbit and also the evolution of the GWs frequency signal during the inspiral phase.…”

Section: Introductionmentioning

confidence: 99%

Effects of Hadron-Quark Phase Transitions in Hybrid Stars within the NJL Model

et al. 2019

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We study local and non-local Polyakov Nambu-Jona-Lasinio models and analyze their respective phase transition diagram. We construct hybrid stars using the zero temperature limit of the local and non-local versions of Nambu-Jona-Lasinio model for quark matter and the modern GM1(L) parametrization of the non-linear relativistic mean field model for hadronic matter. We compare our models with data from PSR J1614-2230 and PSR J0343+0432 and also from GW170817 and its electromagnetic counterpart GRB170817A and AT2017gfo. We study observational signatures of the appearance of a mixed phase as a result of modeling a phase transition that mimics the Gibbs formalism and compare the results with the sharp first-order phase transition obtained using the Maxwell construction. We also study in detail the g-mode associated with discontinuities in the equation of state, and calculate non-radial oscillation modes using relativistic Cowling approximation.

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Signals in the tidal deformability for phase transitions in compact stars with constraints from GW170817

Cited by 100 publications

References 53 publications

Relativistic hybrid stars with sequential first-order phase transitions and heavy-baryon envelopes

Relativistic hybrid stars with sequential first-order phase transitions and heavy-baryon envelopes

Hadron matter in neutron stars in view of gravitational wave observations

Effects of Hadron-Quark Phase Transitions in Hybrid Stars within the NJL Model

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