High-mass twins &amp; resolution of the reconfinement, masquerade and hyperon puzzles of compact star interiors

Blaschke, D.; Alvarez-Castillo, David

doi:10.1063/1.4938602

Cited by 23 publications

(19 citation statements)

References 49 publications

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“…al. [30] also found twin star solutions by assuming a first order phase transition. Their twin star solutions are located near 2M and have very similar mass-radius relations to the ones found in category I and III.…”

Section: Discussionmentioning

confidence: 95%

“…Depending on the features of the transition between the inner and outer parts of hybrid stars, a so called twin star configuration might arise, i.e. a third family of compact stars appears with alike masses as the second family branch of normal neutron or strange quark stars [21][22][23][24][25][26][27][28][29][30][31]. With space missions such as NICER (Neutron star Interior Composition ExploreR) [32], high-precision X-ray astronomy will be able to offer precise measurements of masses and radii of compact stars [33].…”

Section: Introductionmentioning

confidence: 99%

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Classifications of twin star solutions for a constant speed of sound parameterized equation of state

2018

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We explore the possible mass radius relation of compact stars for the equation of states with a first order phase transition. The low density matter is described by a nuclear matter equation of state resulting from fits to nuclear properties. A constant speed of sound parametrization is used to describe the high density matter phase with the speed of sound c 2 s = 1. A classification scheme of four distinct categories including twin star solutions, i. e. solutions with the same mass but differing radii, is found which are compatible with the M ≥ 2M pulsar mass constraint. We show the dependence of the mass and radius differences on the transition parameters and delineate that higher twin star masses are more likely to be accompanied by large radius differences. These massive twin stars are generated by high values of the discontinuity in the energy density and the lowest possible values of the transition pressure that still result in masses of M ≥ 2M at the maximum of the hadronic branch. arXiv:1707.07524v1 [astro-ph.HE]

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Section: Discussionmentioning

confidence: 95%

Section: Introductionmentioning

confidence: 99%

Classifications of twin star solutions for a constant speed of sound parameterized equation of state

2018

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“…The presence of MTs is synonymous to the existence of a third family [2] of CS in the mass-radius (M − R) diagram. It requires the CS EoS to feature a strong first order phase transition from hadron to quark matter [3][4][5][6][7][8], where the latent heat of the transition fulfils the Seidov criterion [9].…”

Section: Introductionmentioning

confidence: 99%

Bayesian Analysis for Extracting Properties of the Nuclear Equation of State from Observational Data Including Tidal Deformability from GW170817

et al. 2019

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We develop a Bayesian analysis method for selecting the most probable equation of state under a set of constraints from compact star physics, which now include the tidal deformability from GW170817. We apply this method for the first time to a two-parameter family of hybrid equations of state that is based on realistic models for the hadronic phase (KVORcut02) and the quark matter phase (SFMα) which produce a third family of hybrid stars in the mass-radius diagram. One parameter (α) characterizes the screening of the string tension in the string-flip model of quark matter while the other (∆ P ) belongs to the mixed phase construction that mimics the thermodynamics of pasta phases and includes the Maxwell construction as a limiting case for ∆ P = 0. We present the corresponding results for compact star properties like mass, radius and tidal deformabilities and use empirical data for them in the newly developed Bayesian analysis method to obtain the probabilities for the model parameters within their considered range.

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“…This possibility of high-mass twin stars is of great importance not only due to the possibility of identification of a critical endpoint in the QCD phase diagram [16,17] but also because it provides a solution to several issues discussed in [18]: the hyperon puzzle [19], the masquerade problem [20] and the reconfinement case [21,22]. Moreover, the transition between twin stars bears an energy reservoir [23] that qualifies it as a possible engine for most energetic explosive astrophysical phenomena like gammaray bursts and fast radio bursts or play a role in contributing to the complex mechanism of core collapse supernova explosions.…”

Section: Introductionmentioning

confidence: 99%

New class of hybrid EoS and Bayesian M - R data analysis

et al. 2016

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Abstract. We explore systematically a new class of two-phase equations of state (EoS) for hybrid stars that is characterized by three main features : (1) stiffening of the nuclear EoS at supersaturation densities due to quark exchange effects (Pauli blocking) between hadrons, modelled by an excluded volume correction, (2) stiffening of the quark matter EoS at high densities due to multiquark interactions and (3) possibility for a strong first order phase transition with an early onset and large density jump. The third feature results from a Maxwell construction for the possible transition from the nuclear to a quark matter phase and its properties depend on the two parameters used for (1) and (2), respectively. Varying these two parameters one obtains a class of hybrid EoS that yields solutions of the Tolman-Oppenheimer-Volkoff (TOV) equations for sequences of hadronic and hybrid stars in the mass-radius diagram which cover the full range of patterns according to the Alford-Han-Prakash classification following which a hybrid star branch can be either absent, connected or disconnected with the hadronic one. The latter case often includes a tiny connected branch. The disconnected hybrid star branch, also called "third family", corresponds to highmass twin stars characterized by the same gravitational mass but different radii. We perform a Bayesian analysis and demonstrate that the observation of such a pair of high-mass twin stars would have a sufficient discriminating power to favor hybrid EoS with a strong first order phase transition over alternative EoS. PACS

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High-mass twins & resolution of the reconfinement, masquerade and hyperon puzzles of compact star interiors

Cited by 23 publications

References 49 publications

Classifications of twin star solutions for a constant speed of sound parameterized equation of state

Classifications of twin star solutions for a constant speed of sound parameterized equation of state

Bayesian Analysis for Extracting Properties of the Nuclear Equation of State from Observational Data Including Tidal Deformability from GW170817

New class of hybrid EoS and Bayesian M - R data analysis

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