Noncongruence of the nuclear liquid-gas and deconfinement phase transitions

Hempel, Matthias; Dexheimer, V.; Schramm, Stefan; Iosilevskiy, Igor

doi:10.1103/physrevc.88.014906

Cited by 92 publications

(106 citation statements)

References 122 publications

(263 reference statements)

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“…[32,33,40,42], it was shown that the slope dP=dTj PT is negative for the QCD phase transition and positive for the liquid-gas phase transition of nuclear matter (see also Refs. [35,36,43]).…”

Section: Relation To the Qcd Phase Diagrammentioning

confidence: 99%

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Hot third family of compact stars and the possibility of core-collapse supernova explosions

et al. 2016

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A phase transition to quark matter can lead to interesting phenomenological consequences in corecollapse supernovae, e.g., triggering an explosion in spherically symmetric models. However, until now, this explosion mechanism was only shown to be working for equations of state that are in contradiction with recent pulsar mass measurements. Here, we identify that this explosion mechanism is related to the existence of a third family of compact stars. For the equations of state investigated, the third family is only pronounced in the hot, early stages of the protocompact star and absent or negligibly small at zero temperature and thus represents a novel kind of third family. This interesting behavior is a result of unusual thermal properties induced by the phase transition, e.g., characterized by a decrease of temperature with increasing density for isentropes, and can be related to a negative slope of the phase transition line in the temperature-pressure phase diagram.

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Section: Relation To the Qcd Phase Diagrammentioning

confidence: 99%

“…The reason for this special property of the QCD phase transition can be identified by using the ClausiusClapeyron equation [27,32,33,40,43],…”

Section: Relation To the Qcd Phase Diagrammentioning

confidence: 99%

Hot third family of compact stars and the possibility of core-collapse supernova explosions

et al. 2016

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“…Therefore, , which is the opposite of its behavior in the nuclear liquid-gas phase transition, sometimes called an "entropic" phase transition (cf. Hempel et al 2013;Iosilevskiy 2013, Iosilevskiy 2015 andreferences therein). This property could lead to interesting consequences for neutron stars and core-collapse supernovae Yudin et al 2016).…”

Section: Bdcmentioning

confidence: 99%

Simultaneous Chiral Symmetry Restoration and Deconfinement Consequences for the QCD Phase Diagram

Klähn

Fischer

Hempel

2017

ApJ

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For studies of quark matter in astrophysical scenarios, the thermodynamic bag model is commonly employed. Although successful, it does not account for dynamical chiral symmetry breaking and repulsions due to the vector interaction which is crucial to explain recent observations of massive, two solar mass neutron stars. In Klähn & Fischer we developed the novel vBag quark matter model which takes these effects into account. This article extends vBag to finite temperatures and isospin asymmetry. Another particular feature of vBag is the determination of the deconfinement bag constant B dc from a given hadronic equation of state in order to ensure that chiral and deconfinement transitions coincide. We discuss consequences of this novel approach for the phase transition construction, the phase diagram, and implications for protoneutron stars.

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“…For this purpose, we extended the hadronic SU(3) non-linear realization of the sigma model, see e.g. [20,21,22,23], to include quark degrees of freedom in a spirit similar to the PNJL model ( [24]), in the sense that it uses the Polyakov loop Φ as the order parameter for deconfinement. The Lagrangian density of the model in mean field approximation reads:…”

Section: Magnetized Equation Of Statementioning

confidence: 99%

Effects of strong magnetic fields on hybrid stars

Franzon¹,

Dexheimer²,

Schramm³

2016

Proceedings of the Modern Physics of Compact Stars 2015 — PoS(MPCS2015)

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In this work we study the effects of strong magnetic fields on hybrid stars by using a full general-relativity approach, solving the coupled Maxwell-Einstein equation in a selfconsistent way. The magnetic field is assumed to be axi-symmetric and poloidal. We take into consideration the anisotropy of the energy-momentum tensor due to the magnetic field, magnetic field effects on equation of state, the interaction between matter and the magnetic field (magnetization), and the anomalous magnetic moment of the hadrons. The equation of state used is an extended hadronic and quark SU(3) non-linear realization of the sigma model that describes magnetized hybrid stars containing nucleons, hyperons and quarks. According to our results, the effects of the magnetization and the magnetic field on the EoS do not play an important role on global properties of these stars. On the other hand, the magnetic field causes the central density in these objects to be reduced, inducing major changes in the populated degrees of freedom and, potentially, converting a hybrid star into a hadronic star.

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Noncongruence of the nuclear liquid-gas and deconfinement phase transitions

Cited by 92 publications

References 122 publications

Hot third family of compact stars and the possibility of core-collapse supernova explosions

Hot third family of compact stars and the possibility of core-collapse supernova explosions

Simultaneous Chiral Symmetry Restoration and Deconfinement Consequences for the QCD Phase Diagram

Effects of strong magnetic fields on hybrid stars

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