Proto–Neutron and Neutron Stars in a Chiral SU(3) Model

Dexheimer, V.; Schramm, Stefan

doi:10.1086/589735

Cited by 216 publications

(221 citation statements)

References 25 publications

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“…Therefore, there has to be a mechanism that suppresses (or removes) the amount of hyperons at densities relevant for compact star physics. One possibility is the vector repulsion of hyperons generated by the exchange of the φ meson [3][4][5]. This finding reinforces the point that when including hyperons as parts of the baryon octet, one should also take into account the corresponding SU(3) multiplets in the meson sector.…”

Section: Modeling Compact Starssupporting

confidence: 65%

Dense and hot matter in compact stars and heavy-ion collisions

Schramm¹,

Dexheimer

Mukherjee³

et al. 2018

EPJ Web Conf.

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Abstract. We discuss the effect of exotic particles in neutron star matter and the corresponding impact on gross properties of neutron stars within effective models for the strong interaction. Particularly, for the quark-hadron parity-doublet model, we show results for compact star properties and discuss the phase structure of the model and its possible relevance for heavy-ion collision phenomenology.

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Section: Modeling Compact Starssupporting

confidence: 65%

Dense and hot matter in compact stars and heavy-ion collisions

Schramm¹,

Dexheimer

Mukherjee³

et al. 2018

EPJ Web Conf.

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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%

“…The later is important in order to reproduce a realistic structure for the QCD phase diagram over the whole range of chemical potentials and temperatures, including realistic thermodynamic behaviour at vanishing chemical potential as shown in [22]. The effective masses of the baryons and quarks are generated by the scalar mesons except for a small explicit mass term M 0 and the term containing Φ:…”

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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“…A detailed discussion of the model and specific values of the parameters can be found in [14]. In order to study compact stars we determine the equation of state within this model and solve the Tolman-Oppenheimer-Volkoff equations for static stars [15,16].…”

Section: The Quark-hadron (Qh) Modelmentioning

confidence: 99%

Structure and Cooling of Neutron and Hybrid Stars

Schramm

Dexheimer

Negreiros

et al. 2013

Exciting Interdisciplinary Physics

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The study of neutron stars is a topic of central interest in the investigation of the properties of strongly compressed hadronic matter. Whereas in heavy-ion collisions the fireball, created in the collision zone, contains very hot matter, with varying density depending on the beam energy, neutron stars largely sample the region of cold and dense matter with the exception of the very short time period of the existence of the proto-neutron star. Therefore, neutron star physics, in addition to its general importance in astrophysics, is a crucial complement to heavy-ion physics in the study of strongly interacting matter. In the following, model approaches will be introduced to calculate properties of neutron stars that incorporate baryons and quarks. These approaches are also able to describe the state of matter over a wide range of temperatures and densities, which is essential if one wants to connect and correlate star observables and results from heavy-ion collisions. The effect of exotic particles and quark cores on neutron star properties will be considered. In addition to the gross properties of the stars like their masses and radii their expected inner composition is quite sensitive to the models used. The effect of the composition can be studied through the analysis of the cooling curve of the star. In addition, we consider the effect of rotation, as in this case the particle composition of the star can be modified quite drastically.

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Proto–Neutron and Neutron Stars in a Chiral SU(3) Model

Cited by 216 publications

References 25 publications

Dense and hot matter in compact stars and heavy-ion collisions

Dense and hot matter in compact stars and heavy-ion collisions

Effects of strong magnetic fields on hybrid stars

Structure and Cooling of Neutron and Hybrid Stars

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