Constraining twin stars with GW170817

Montaña, Glòria; Tolós, Laura; Hanauske, Matthias; Rezzolla, Luciano

doi:10.1103/physrevd.99.103009

Cited by 183 publications

(170 citation statements)

References 131 publications

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“…Fi and of the Fermi momentum k Fi = (µ i + vec 2 − M * i 2 ), together with Eqs. (5) and (11) to write a general relation connecting electron and charged chemical potential n max T max We used "vec" referring to general vector interactions, but they are specified in Eq. (4) for our model.…”

Section: Resultsmentioning

confidence: 99%

On the deconfinement phase transition in neutron-star mergers

et al. 2020

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We study in detail the nuclear aspects of a neutron-star merger in which deconfinement to quark matter takes place. For this purpose, we make use of the Chiral Mean Field (CMF) model, an effective relativistic model that includes self-consistent chiral symmetry restoration and deconfinement to quark matter and, for this reason, predicts the existence of different degrees of freedom depending on the local density/chemical potential and temperature. We then use the out-of-chemical-equilibrium finite-temperature CMF equation of state in full general-relativistic simulations to analyze which regions of different QCD phase diagrams are probed and which conditions, such as strangeness and entropy, are generated when a strong first-order phase transition appears. We also investigate the amount of electrons present in different stages of the merger and discuss how far from chemical equilibrium they can be and, finally, draw some comparisons with matter created in supernova explosions and heavy-ion collisions.PACS. PACS-key discribing text of that key -PACS-key discribing text of that key

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Section: Resultsmentioning

confidence: 99%

On the deconfinement phase transition in neutron-star mergers

et al. 2020

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“…However, it is possible to regain stability at higher central pressure (solid line) resulting in a second stable branch (or the "third family" of compact stars) if the parameters p 1 , ∆ε 1 and s 1 are chosen appropriately. In particular in this case, twin configurations appear where two stars have the same masses but different radii [6,[11][12][13][14]. If a second phase transition in the quark phase takes place then a third stable branch (or fourth family) of compact stars containing Q2 quark matter in the core arises.…”

Section: B Quark Matter Eosmentioning

confidence: 99%

“…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%

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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“…The GW170817 event detected by LIGO [11] is the first confirmed merger event of compact stars. Together with the subsequent detection of the electromagnetic counterpart, GRB 170817A and AT2017gfo [12], they lead us to the era of "multi-messenger astronomy", which has inspired a lot of studies that greatly move our understanding of nuclear matter forward [13][14][15][16][17][18][19][20][21][22][23][24][25][26]. The chirp mass of the binary is determined to be M c = 1.188 M .…”

Section: Introductionmentioning

confidence: 99%

Probing up-down quark matter via gravitational waves

Zhang

2020

Phys. Rev. D

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Recently, it was shown that quark matter with only u, d quarks (udQM) can be the ground state of matter for baryon number A > Amin with Amin 300. In this paper, we explore ud quark stars (udQSs) that are composed of udQM, in the context of the two-families scenario in which udQSs and hadronic stars (HSs) can co-exist. Distinct signatures are discussed compared to the conventional study regarding strange quark stars (SQSs). We show that the requirements of Amin 300 and the most-massive compact star observed being udQS together put stringent constraints on the allowed parameter space of udQSs. Then we study the related gravitational-wave probe of the tidal deformability in binary star mergers, including the udQS-udQS and udQS-HS cases. The obtained values of the tidal deformability at 1.4 solar mass and the average tidal deformability are all in good compatibility with the experimental constraints of GW170817/AT2017gfo. This study points to a new possible interpretation of the GW170817 binary merger event, where udQS may be at least one component of the binary system detected.

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Constraining twin stars with GW170817

Cited by 183 publications

References 131 publications

On the deconfinement phase transition in neutron-star mergers

On the deconfinement phase transition in neutron-star mergers

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

Probing up-down quark matter via gravitational waves

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