Stellar core collapse with hadron-quark phase transition

Nakazato, Ken’ichiro; Sumiyoshi, Kohsuke; Yamada, Shoichi

doi:10.1051/0004-6361/201322231

Cited by 25 publications

(24 citation statements)

References 18 publications

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“…The latter models are labeled "STOSQxxxn" for the one with quarks and "STOSQxxxnπ" for the one with quarks and pions. Nakazato, Sumiyoshi, and Yamada (2013) Yamada (2008, 2013). The thermodynamic properties are strongly influenced by the possible existence of quark matter at high densities and temperatures and, in particular, the phase transition can have an important effect on the dynamics of CCSNe (see Sec.…”

Section: Including Additional Degrees Of Freedommentioning

confidence: 99%

“…In the subsequent works exploring this scenario [see, e.g., Sagert et al (2010), Fischer et al (2011Fischer et al ( , 2012, Nakazato, Sumiyoshi, and Yamada (2013), ], explosions could not be obtained if the maximum mass of the employed EoS is sufficiently high. It is clear that the required stiffening in the quark phase to reach 2M ⊙ typically does not allow for a strong first-order phase transition that seems to be necessary in this scenario to trigger explosions.…”

Section: Dynamicsmentioning

confidence: 99%

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Equations of state for supernovae and compact stars

et al. 2017

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A review is given of various theoretical approaches for the equation of state (EoS) of dense matter, relevant for the description of core-collapse supernovae, compact stars, and compact star mergers. The emphasis is put on models that are applicable to all of these scenarios. Such EoS models have to cover large ranges in baryon number density, temperature, and isospin asymmetry. The characteristics of matter change dramatically within these ranges, from a mixture of nucleons, nuclei, and electrons to uniform, strongly interacting matter containing nucleons, and possibly other particles such as hyperons or quarks. As the development of an EoS requires joint efforts from many directions, different theoretical approaches are considered and relevant experimental and observational constraints which provide insights for future research are discussed. Finally, results from applications of the discussed EoS models are summarized.

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Section: Including Additional Degrees Of Freedommentioning

confidence: 99%

Section: Dynamicsmentioning

confidence: 99%

Equations of state for supernovae and compact stars

et al. 2017

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“…Only for detailed comparisons, the exact M-R relations have to be calculated with the strange quark mass taken into account. [30,32]. They did not consider corrections from strong interactions, and therefore obtain maximum masses only below 2 M ⊙ .…”

Section: Quark Eos Modelsmentioning

confidence: 99%

“…However, the hybrid EOSs applied in [25] have maximum masses much below 2 M ⊙ . In the subsequent works exploring this scenario [25][26][27][28][29][30][31], explosions could not be obtained if the maximum mass was sufficiently high.…”

Section: Introductionmentioning

confidence: 99%

Towards generating a new supernova equation of state: A systematic analysis of cold hybrid stars

Heinimann¹,

Hempel²,

Thielemann³

2016

Phys. Rev. D

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The hadron-quark phase transition in core-collapse supernovae (CCSNe) has the potential to trigger explosions in otherwise nonexploding models. However, those hybrid supernova equations of state (EOS) shown to trigger an explosion do not support the observational 2 M ⊙ neutron star maximum mass constraint. In this work, we analyze cold hybrid stars by the means of a systematic parameter scan for the phase transition properties, with the aim to develop a new hybrid supernova EOS. The hadronic phase is described with the state-of-the-art supernova EOS HS(DD2), and quark matter by an EOS with a constant speed of sound (CSS) of c 2 QM ¼ 1=3. We find promising cases which meet the 2 M ⊙ criterion and are interesting for CCSN explosions. We show that the very simple CSS EOS is transferable into the wellknown thermodynamic bag model, important for future application in CCSN simulations. In the second part, the occurrence of reconfinement and multiple phase transitions is discussed. In the last part, the influence of hyperons in our parameter scan is studied. Including hyperons no change in the general behavior is found, except for overall lower maximum masses. In both cases (with and without hyperons) we find that quark matter with c 2 QM ¼ 1=3 can increase the maximum mass only if reconfinement is suppressed or if quark matter is absolutely stable.

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“…Some EoSs also consider a phase transition to quark matter. The MIT bag model is applied, e.g., in [332,333,413,414,154,153], and the transition from hadronic to quark phase is modelled with a Gibbs construction.…”

Section: General Purpose Equations Of Statementioning

confidence: 99%

Nuclear Equation of State for Compact Stars and Supernovae

Burgio

Fantina

2018

Astrophysics and Space Science Library

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The equation of state (EoS) of hot and dense matter is a fundamental input to describe static and dynamical properties of neutron stars, core-collapse supernovae and binary compact-star mergers. We review the current status of the EoS for compact objects, that have been studied with both ab-initio many-body approaches and phenomenological models. We limit ourselves to the description of EoSs with purely nucleonic degrees of freedom, disregarding the appearance of strange baryonic matter and/or quark matter. We compare the theoretical predictions with different data coming from both nuclear physics experiments and astrophysical observations. Combining the complementary information thus obtained greatly enriches our insight into the dense nuclear matter properties. Current challenges in the description of the EoS are also discussed, mainly focusing on the model dependence of the constraints extracted from either experimental or observational data, the lack of a consistent and rigorous many-body treatment at zero and finite temperature of the matter encountered in compact stars (e.g. problem of cluster formation and extension of the EoS to very high temperatures), the role of nucleonic three-body forces, and the dependence of the direct URCA processes on the EoS.

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Stellar core collapse with hadron-quark phase transition

Cited by 25 publications

References 18 publications

Equations of state for supernovae and compact stars

Equations of state for supernovae and compact stars

Towards generating a new supernova equation of state: A systematic analysis of cold hybrid stars

Nuclear Equation of State for Compact Stars and Supernovae

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