Equations of state for supernovae and compact stars

By M. Oertel, M. Hempel, T. Klähn, S. Typel. 2016

684 citations recorded by the source corpus.

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.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/2e1cc1fbbff7a36d56eb54395698bb013f4efb76

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Citations in the corpus

Symmetry Parameter Constraints from a Lower Bound on Neutron-matter Energy (2016, background): “Other experimental constraints on symmetry energy parameters are reviewed in Lattimer & Lim (2013) and Oertel et al. (2017).”
Progress in Constraining Nuclear Symmetry Energy Using Neutron Star Observables Since GW170817 (2021, background): “The slope parameter L of nuclear symmetry symmetry from (1) 2013 survey of 29 analyses of terrestrial experiments and astrophysical observations (between the dashed blue lines) [54], (2) 2016 surveys of 53 analyses (between the violet lines) [8] and (3) 24 new analyses of neutron star observables si”
Evidence for a maximum mass cut-off in the neutron star mass distribution and constraints on the equation of state (2017, background): “This set of EoS tables is not intended to be exhaustive: for a more complete catalog, see e.g. Oertel et al. (2017).”
Constraining the Dense Matter Equation of State with Joint Analysis of NICER and LIGO/Virgo Measurements (2019, background): “…span a wide range, from neutron-rich nucleonic matter to hyperon or deconfined quark formation or the emergence of a Bose-Einstein condensate or a color superconducting phase (see Hebeler et al. 2015; Lattimer & Prakash 2016; Oertel et al. 2017; Baym et al. 2018, for recent reviews on this topic).”
Origin of the heaviest elements: The rapid neutron-capture process (2019, methodology): “IMA treatments Ojima et al. (2018), utilizing a variation of sizes of such galactic substructures, made use of related different star formation rates and different outflows according to their gravity, and added stochastically neutron star mergers in these substructures within the range of possible c”
Neutron-star Radius Constraints from GW170817 and Future Detections (2017, background): “Apart from the importance of this detection for stellar astrophysics and nucleosynthesis, such events are highly interesting because they bear the potential to infer weakly-constrained properties of NSs (Lattimer & Prakash 2016; Özel & Freire 2016; Oertel et al. 2017).”
Using Gravitational-wave Observations and Quasi-universal Relations to Constrain the Maximum Mass of Neutron Stars (2017, result): “Third, the results presented here already have a direct impact on some of the EOSs describing matter at nuclear densities (see, e.g., Oertel et al. (2017) for a recent review).”
Combined Constraints on the Equation of State of Dense Neutron-rich Matter from Terrestrial Nuclear Experiments and Observations of Neutron Stars (2018, background): “(Lattimer & Prakash 2016; Oertel et al. 2017; Özel & Freire 2016; Watts et al. 2016; Grigorian et al. 2016; Newton et al. 2014) for recent reviews.”