Consequences of a strong phase transition in the dense matter equation of state for the rotational evolution of neutron stars

Bejger, M.; Blaschke, D.; Haensel, P.; Zdunik, J. L.; Fortin, M.

doi:10.1051/0004-6361/201629580

Cited by 43 publications

(38 citation statements)

References 90 publications

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“…Comparing the gravitational masses of these two star configurations one can estimate the release of binding energy in this process, see Ref. [35]. Figure 7.…”

Section: Compact Star Sequencesmentioning

confidence: 99%

Two Novel Approaches to the Hadron-Quark Mixed Phase in Compact Stars

et al. 2018

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First-order phase transitions, like the liquid-gas transition, proceed via formation of structures such as bubbles and droplets. In strongly interacting compact star matter, at the crust-core transition, but also at the hadron-quark transition in the core, these structures form different shapes dubbed "pasta phases". We describe two methods to obtain one-parameter families of hybrid equations of state (EoS) which mimic the thermodynamic behavior of pasta phases in between a low-density hadron and a high-density quark matter phase, thus generalizing the Maxwell construction. The first method replaces the behavior of pressure vs. chemical potential in a finite region around the critical pressure of the Maxwell construction by a polynomial interpolation. The second method uses extrapolations of the hadronic and quark matter EoS beyond the Maxwell point to define a mixing of both with weight functions bounded by finite limits around the Maxwell point. We apply both methods to the case of a hybrid EoS with a strong first order transition that entails the formation of a third family of compact stars and the corresponding mass twin phenomenon. We investigate for both models the robustness of this phenomenon against variation of the single parameter, the pressure increment at the critical chemical potential which quantifies the deviation from the Maxwell construction. We also show sets of results for other compact star observables than mass and radius, namely the moment of inertia and the baryon mass.

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“…Comparing the gravitational masses of these two star configurations one can estimate the release of binding energy in this process, see Ref. [35]. Figure 7.…”

Section: Compact Star Sequencesmentioning

confidence: 99%

Two Novel Approaches to the Hadron-Quark Mixed Phase in Compact Stars

et al. 2018

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“…One scenario involves a spin-up (in a binary) or spin-down (in isolation) induced QCD phase transition in a compact star which would be accompanied by a quick change in the star's global properties. This could induce drastic (depending on how large the energy-density jump is) changes in spin, for example, backbending [47][48][49], or a release of large portions of gravitational binding energy in an explosion or collapse [50][51][52]. Core-collapse supernovas provide yet another setting where the QCD phase transition(s) can induce additional shock wave(s) [53] and affect the supernova outcome.…”

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confidence: 99%

Compact Stars with Sequential QCD Phase Transitions

2017

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Compact stars may contain quark matter in their interiors at densities exceeding several times the nuclear saturation density. We explore models of such compact stars where there are two first-order phase transitions: the first from nuclear matter to a quark-matter phase, followed at a higher density by another first-order transition to a different quark-matter phase [e.g., from the two-flavor color-superconducting (2SC) to the color-flavor-locked (CFL) phase]. We show that this can give rise to two separate branches of hybrid stars, separated from each other and from the nuclear branch by instability regions, and, therefore, to a new family of compact stars, denser than the ordinary hybrid stars. In a range of parameters, one may obtain twin hybrid stars (hybrid stars with the same masses but different radii) and even triplets where three stars, with inner cores of nuclear matter, 2SC matter, and CFL matter, respectively, all have the same mass but different radii.

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“…See Refs. [4,5,6] and references therein for studies of the relation of magnetic field strengths, temperature and rotation in the evolution of neutron stars. As has been discussed in Refs.…”

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What is the magnetic field distribution for the equation of state of magnetized neutron stars?

et al. 2017

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In this Letter, we report a realistic calculation of the magnetic field profile for the equation of state inside strongly magnetized neutron stars. Unlike previous estimates, which are widely used in the literature, we find that magnetic fields increase relatively slowly with increasing baryon chemical potential (or baryon density) of magnetized matter. More precisely, the increase is polynomial instead of exponential, as previously assumed. Through the analysis of several different realistic models for the microscopic description of stellar matter (including hadronic, hybrid and quark models) combined with general relativistic solutions endowed with a poloidal magnetic field obtained by solving Einstein-Maxwell's field equations in a self-consistent way, we generate a phenomenological fit for the magnetic field distribution in the stellar polar direction to be used as input in microscopic calculations.

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Consequences of a strong phase transition in the dense matter equation of state for the rotational evolution of neutron stars

Cited by 43 publications

References 90 publications

Two Novel Approaches to the Hadron-Quark Mixed Phase in Compact Stars

Two Novel Approaches to the Hadron-Quark Mixed Phase in Compact Stars

Compact Stars with Sequential QCD Phase Transitions

What is the magnetic field distribution for the equation of state of magnetized neutron stars?

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