The Quest for the Nuclear Equation of State

Aichelin, J.; Schaffner–Bielich, Jürgen

doi:10.1007/978-3-642-01539-7_4

Cited by 4 publications

(5 citation statements)

References 120 publications

(124 reference statements)

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“…In this scheme, the only input quantity we need is the bare NN interaction v in the Bethe-Goldstone equation (1). The nuclear EoS can be calculated with good accuracy in the Brueckner two hole-line approximation with the continuous choice for the single-particle potential, since the results in this scheme are quite close to the calculations which include also the three hole-line contribution [17].…”

Section: A the Brueckner-bethe-goldstone Approachmentioning

confidence: 97%

“…The experimental data on heavy ion collisions have been systematically analyzed on the basis of detailed simulations, in order to constrain not only the density dependence of the EoS, but also its isospin dependence. Excellent reviews on this subject can be found in the literature [1,2]. On the other hand, the analysis of astrophysical observational data, noticeably on compact objects, are of great relevance for the study of the nuclear EoS.…”

Section: Introductionmentioning

confidence: 99%

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Selecting microscopic equations of state

2013

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We compare a set of equations of state derived within microscopic many-body approaches, and study their predictions as far as phenomenological data on nuclei from heavy ion collisions, and astrophysical observations on neutron stars are concerned. We find that all the data, taken together, put strong constraints not easy to be fulfilled accurately. However, no major discrepancies are found among the selected equations of state and with respect to the data. The results provide an estimate of the uncertainty on the theoretical prediction at a microscopic level of the nuclear equation of state.

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Section: A the Brueckner-bethe-goldstone Approachmentioning

confidence: 97%

Section: Introductionmentioning

confidence: 99%

Selecting microscopic equations of state

2013

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“…Consequences of these constraints from HICs on compact star properties were explored by Sagert, Tolos et al (2012). For a discussion of the interplay between HICs and astrophysical data see, e.g., Aichelin and Schaffner-Bielich (2009).…”

Section: Heavy-ion Collisionsmentioning

confidence: 99%

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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“…Hence, kaons can escape from the high density zone unimpeded, their production rates will be controlled by the amount of compression achieved in the central region of the collision. For a recent review of the relation between the nuclear equation of state and kaon production rates in heavy-ion collisions see [29].…”

Section: Maximum Possible Mass Of Neutron Starsmentioning

confidence: 99%

Strangeness in Compact Stars

Schaffner-Bielich

2010

Nuclear Physics A

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We discuss the impact of strange hadrons, in particular hyperons, on the gross features of compact stars and on core-collapse supernovae. Hyperons are likely to be the first exotic species which appears around twice normal nuclear matter density in the core of neutron stars. Their presence largely influences the mass-radius relation of compact stars, the maximum mass, the cooling of neutron stars, the stability with regard to the emission of gravitational waves from rotationpowered neutron stars and the possible early onset of the QCD phase transition in core-collapse supernovae. We outline also the constraints from subthreshold kaon production in heavy-ion collisions for the maximum possible mass of neutron stars.

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The Quest for the Nuclear Equation of State

Abstract: The present status of the efforts to determine the nuclear equation of state from results of heavy ion reactions and from astrophysical observations is reviewed.

Cited by 4 publications

References 120 publications

Selecting microscopic equations of state

Selecting microscopic equations of state

Equations of state for supernovae and compact stars

Strangeness in Compact Stars

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