Maximum latent heat of neutron star matter independent of general relativity

Lope-Oter, Eva; Llanes-Estrada, Felipe J.

doi:10.1103/physrevc.105.l052801

Cited by 12 publications

(7 citation statements)

References 27 publications

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“…We choose only one parametrization since they yield qualitatively similar results. One can see that our results for the latent energy at zero temperature are of the same order of magnitude as the ones obtained in [63], but never reach the values shown in [65] and are always positive. As far as the latent heat is concerned, the behaviour we find is more similar to the result shown in [66] and we do find a maximum point, but at much lower temperatures.…”

Section: Latent Heat and Latent Energysupporting

confidence: 54%

QCD phase diagrams via QHD and MIT based models

Biesdorf¹,

Lopes²,

Menezes³

2023

Preprint

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In this paper, the QCD phase diagram is obtained from the crossing of two effective models: the MIT bag based models are used to describe quark matter and QHD type models to describe hadronic matter. We use the Gibbs' conditions to establish the crossing points of the pressure in function of the chemical potential obtained in both phases. We first analyze two-flavour symmetric matter constrained to both the freeze-out and the liquid-gas phase transition at the hadronic phase. Later we analyse the results for β-stable and charge neutral stellar matter and compare two different prescriptions: one that assumes flavour conservation, so that the quark phase is completely determined from the hadronic phase, and the other based on the Maxwell construction, where the quark phase is also β-stable. At the end, we compute the latent heat to find a signature of the critical end point.

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Section: Latent Heat and Latent Energysupporting

confidence: 54%

QCD phase diagrams via QHD and MIT based models

Biesdorf¹,

Lopes²,

Menezes³

2023

Preprint

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“…Testing modified theories of gravity requires a prior knowledge of the equation of state of the dense matter, and thus, constraints independent of the gravitational theories could play a crucial role in the understanding of the properties of the neutron stars. In [105] it was proposed to use the function we propose the function L|…”

Section: Discussion and Final Remarksmentioning

confidence: 99%

“…the indices E and H refer to the exotic and hadronic phases, respectively, as a diagnostic tool for constraining the equation of state of dense matter in a first order phase transition. The existence of a family of latent-heat maxima to constrain the equation of state of neutron matter, is relevant even in modified theories of gravity [105]. Moreover, latent heat is a significant characteristic of the equation of state in cold QCD.…”

Section: Discussion and Final Remarksmentioning

confidence: 99%

Compact stellar structures in Weyl geometric gravity

Haghani¹,

Harkó²

2023

Preprint

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We consider the structure and physical properties of specific classes of neutron, quark, and Bose-Einstein Condensate stars in the conformally invariant Weyl geometric gravity theory. The basic theory is derived from the simplest conformally invariant action, constructed, in Weyl geometry, from the square of the Weyl scalar, the strength of the Weyl vector, and a matter term, respectively. The action is linearized in the Weyl scalar by introducing an auxiliary scalar field. To keep the theory conformally invariant the trace condition is imposed on the matter energy-momentum tensor. The field equations are derived by varying the action with respect to the metric tensor, Weyl vector field and scalar field. By adopting a static spherically symmetric interior geometry, we obtain the field equations, describing the structure and properties of stellar objects in Weyl geometric gravity. The solutions of the field equations are obtained numerically, for different equations of state of the neutron and quark matter. More specifically, constant density stellar models, and models described by the stiff fluid, radiation fluid, quark bag model, and Bose-Einstein Condensate equations of state are explicitly constructed numerically in both general relativity and Weyl geometric gravity, thus allowing an in depth comparison between the predictions of these two gravitational theories. As a general result it turns out that for all the considered equations of state, Weyl geometric gravity stars are more massive than their general relativistic counterparts. As a possible astrophysical application of the obtained results we suggest that the recently observed neutron stars, with masses in the range of 2M⊙ and 3M⊙, respectively, could be in fact conformally invariant Weyl geometric neutron or quark stars.

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“…as proposed in [64], which quantifies the intensity of the phase transition, i.e., the discontinuity in the energy density between phases. The latent heat diminishes in magnetized matter, more prominently for smaller bag values.…”

Section: Phase Transitionmentioning

confidence: 99%

“…The importance of the magnetic field on the strong interactions is long known, as it may alter the transition temperature, chemical potential and latent heat of the deconfinement phase transition, modify the vacuum structure, the dynamic quark masses and the chiral transition [57][58][59][60][61][62]. The latent heat is an important ingredient as it quantifies the discontinuity in the energy density [63] and general upper bounds have been derived from nuclear physics alone [64], being applicable to effective models and to modified general relativity theories. Moreover, it also indicates the point where the transition changes from a first order to a crossover at finite temperatures, when its value is zero [62], a feature expected in the QCD phase diagram, where the critical end point is expected to exist [65].…”

Section: Introductionmentioning

confidence: 99%

Phase transitions and latent heat in magnetized matter

Pelicer¹,

Menezes²

2022

Preprint

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Based on the assumption that the QCD phase diagram gives a realistic picture of hadronic and quark matter under different regimes, it is possible to claim that a quark core may be present inside compact objects commonly named hybrid neutron stars or even that a pure strange star may exist. In this work we explore how the phase transition is modified by the presence of strong magnetic fields and how it is impacted by parameters of the quark phase, for which we use the MIT-model with vector interactions. The phase transition is assumed to conserve flavor when hadrons turn into deconfined quarks. The hadronic equation of state is calculated with the NL3ωρ * parametrization of quantum hadrodynamics. We find that the magnetic field slightly reduces the pressure and chemical potential of the phase transition and the latent heat, the latter being very model dependent.

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Maximum latent heat of neutron star matter independent of general relativity

Cited by 12 publications

References 27 publications

QCD phase diagrams via QHD and MIT based models

QCD phase diagrams via QHD and MIT based models

Compact stellar structures in Weyl geometric gravity

Phase transitions and latent heat in magnetized matter

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