Nonextensive statistical effects in protoneutron stars

Lavagno, Andrea; Pigato, Daniele

doi:10.1140/epja/i2011-11052-1

Cited by 101 publications

(76 citation statements)

References 59 publications

(56 reference statements)

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“…In this context the non-extensive statistical mechanics proposed by Tsallis [1][2][3] can be used to describe and investigate such physical phenomena. Nonextensive statistical effects should strongly affect the finite temperature and nuclear density Equation of State (EOS) [35][36][37][38][39][40]. In fact, by varying temperature and density, the EOS reflects (in terms of the macroscopic thermodynamical variables) the microscopic interactions between the different nuclear matter phases.…”

Section: Introductionmentioning

confidence: 99%

Nonextensive statistical effects in the quark-gluon plasma formation at relativistic heavy-ion collisions energies

Gervino¹,

Lavagno²,

Pigato³

2012

Open Physics

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Abstract:We investigate the relativistic equation of state of hadronic matter and quark-gluon plasma at finite temperature and baryon density in the framework of the non-extensive statistical mechanics, characterized by power-law quantum distributions. We impose the Gibbs conditions on the global conservation of baryon number, electric charge and strangeness number. For the hadronic phase, we study an extended relativistic mean-field theoretical model with the inclusion of strange particles (hyperons and mesons). For the quark sector, we employ an extended MIT-Bag model. In this context we focus on the relevance of non-extensive effects in the presence of strange matter.PACS (2008)

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Section: Introductionmentioning

confidence: 99%

Nonextensive statistical effects in the quark-gluon plasma formation at relativistic heavy-ion collisions energies

Gervino¹,

Lavagno²,

Pigato³

2012

Open Physics

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“…[9], and GM3, from Glendenning and Moszkowski [10]. The above EOSs are compatible with intermediate heavy ion collisions constraints and extensively used in various high density astrophysical applications [11][12][13][14][15][16].…”

Section: The Effective Relativistic Mean Field Modelmentioning

confidence: 99%

Hadron yield ratios in an effective relativistic equation of state

Lavagno

2014

EPJ Web of Conferences

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Abstract. We investigate an effective relativistic equation of state at finite values of temperature and baryon chemical potential with the inclusion of the full octet of baryons, the Delta-isobars and the lightest pseudoscalar and vector meson degrees of freedom. These last particles have been introduced within a phenomenological approach by taking into account of an effective chemical potential and mass depending on the self-consistent interaction between baryons. In this framework, we study of the hadron yield ratios measured in central heavy ion collisions over a broad energy range.

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“…In this direction, many efforts have been focused on searching for possible phase transitions at finite temperature in dense nuclear matter. The knowledge of the nuclear equation of state (EOS) of dense matter at finite temperature plays a crucial role in the determination of the structure and in the evolution of the protoneutron star (PNS) [1][2][3]. A PNS is formed in a stellar remnant after a successful core-collapse supernova explosion of a star with a mass smaller than about 20 solar masses and in the first seconds of its evolution it is a very hot (temperature of up to 50 MeV), lepton rich and β-stable object and a lepton concentration typical of the pre-supernova matter [1,2].…”

Section: Introductionmentioning

confidence: 99%

Nuclear phase transition and thermodynamic instabilities in dense nuclear matter

Lavagno

2018

EPJ Web Conf.

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Abstract. We study the presence of thermodynamic instabilities in a nuclear medium at finite temperature and density where nuclear phase transitions can take place. Such a phase transition is characterized by pure hadronic matter with both mechanical instability (fluctuations on the baryon density) that by chemical-diffusive instability (fluctuations on the electric charge concentration). Similarly to the liquid-gas phase transition, the nucleonic and the ∆-matter phase have a different isospin density in the mixed phase. In the liquid-gas phase transition, the process of producing a larger neutron excess in the gas phase is referred to as isospin fractionation. A similar effects can occur in the nucleon-∆ matter phase transition due essentially to a ∆ − excess in the ∆-matter phase in asymmetric nuclear matter. In this context we also discuss the relevance of ∆-isobar and hyperon degrees of freedom in the bulk properties of the protoneutron stars at fixed entropy per baryon, in the presence and in the absence of trapped neutrinos.

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Nonextensive statistical effects in protoneutron stars

Cited by 101 publications

References 59 publications

Nonextensive statistical effects in the quark-gluon plasma formation at relativistic heavy-ion collisions energies

Nonextensive statistical effects in the quark-gluon plasma formation at relativistic heavy-ion collisions energies

Hadron yield ratios in an effective relativistic equation of state

Nuclear phase transition and thermodynamic instabilities in dense nuclear matter

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