Phase transitions and latent heat in magnetized matter

Pelicer, M. R.; Menezes, D. P.

doi:10.1140/epja/s10050-022-00829-0

Cited by 5 publications

(3 citation statements)

References 87 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: 46%

“…As the contribution to the chemical potential from the leptons is very small, these differences are also very small. From this sub-scenario we choose the one where there is a conservation of the lepton fraction at the point of the phase transition because, in this case, the charge neutrality is also preserved, This approach is contrary to what was done in [63]. We find that this is more compelling to be true than the case where we have the same lepton density at the point of the phase transition, but no charge neutrality.…”

Section: B Stellar Mattermentioning

confidence: 97%

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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: 46%

Section: B Stellar Mattermentioning

confidence: 97%

QCD phase diagrams via QHD and MIT based models

Biesdorf¹,

Lopes²,

Menezes³

2023

Preprint

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“…A strong magnetic field can have several implications for NSs, such as modifying the EoS due to Landau quantization of the constituent charged particles (Landau & Lifshitz 1965;Strickland et al 2012), changing the energy-momentum tensor, and breaking the stellar spherical symmetry. Several studies have shown the effect of the magnetic field on the NS EoS and on stellar properties (Bandyopadhyay et al 1997;Chakrabarty et al 1997;Broderick et al 2000;Felipe et al 2008;Rabhi et al 2008;Casali et al 2014;Mallick & Schramm 2014;Chatterjee et al 2015Chatterjee et al , 2019Sotani & Tatsumi 2015;Fogaça et al 2016;Tolos et al 2016;Gomes et al 2017Gomes et al , 2019Pili et al 2017;Ferrer & Hackebill 2019;Dexheimer et al 2021b;Marquez et al 2022;Pelicer & Menezes 2022). Most of the previous studies that include magnetic field effects on the EoS use isotropic Tolman-Oppenheimer-Volkoff (TOV) equations to determine the relevant stellar properties.…”

Section: Introductionmentioning

confidence: 99%

Magnetic-field Induced Deformation in Hybrid Stars

Rather¹,

Rather

Dexheimer³

et al. 2023

ApJ

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The effects of strong magnetic fields on the deconfinement phase transition expected to take place in the interior of massive neutron stars are studied in detail for the first time. For hadronic matter, the very general density-dependent relativistic mean field model is employed, while the simple, but effective vector-enhanced bag model is used to study quark matter. Magnetic-field effects are incorporated into the matter equation of state and in the general-relativity solutions, which also satisfy Maxwell’s equations. We find that for large values of magnetic dipole moment, the maximum mass, canonical mass radius, and dimensionless tidal deformability obtained for stars using spherically symmetric Tolman–Oppenheimer–Volkoff (TOV) equations and axisymmetric solutions attained through the LORENE library differ considerably. The deviations depend on the stiffness of the equation of state and on the star mass being analyzed. This points to the fact that, unlike what was assumed previously in the literature, magnetic field thresholds for the approximation of isotropic stars and the acceptable use of TOV equations depend on the matter composition and interactions.

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