Equations of state for supernovae and compact stars
Laboratoire Univers et Théories · Délégation Paris 7 · +4 more institutions
Abstract
What are the thermodynamic properties of matter at extreme densities, even exceeding nuclear matter density severely? How can we describe the composition of matter for such conditions, the resulting pressure, and the maximum mass of cold neutron stars? How is this affected by finite temperatures, as they occur in core collapse supernovae and in compact star mergers? This review addresses these points within the framework of constraints from experiments as well as astronomical observations.
Citation impact
- FWCI
- 59.70
- Percentile
- 100%
- References
- 1,086
Authors
4- MOMicaela OertelCorresponding
Laboratoire Univers et Théories, Délégation Paris 7, Université Paris Cité, Université Paris Sciences et Lettres, Centre National de la Recherche Scientifique, Sorbonne Paris Cité
- MHMatthias Hempel
Sorbonne Paris Cité, Université Paris Cité, Délégation Paris 7, Laboratoire Univers et Théories, Centre National de la Recherche Scientifique, Université Paris Sciences et Lettres
- TKT. Klähn
Centre National de la Recherche Scientifique, Université Paris Cité, Laboratoire Univers et Théories, Délégation Paris 7, Sorbonne Paris Cité, Université Paris Sciences et Lettres
- STS. Typel
Centre National de la Recherche Scientifique, Sorbonne Paris Cité, Université Paris Cité, Université Paris Sciences et Lettres, Délégation Paris 7, Laboratoire Univers et Théories
Topics & keywords
- Physics
- Equation of state
- Supernova
- Nucleon
- Hyperon
- Neutron star
- Asymmetry
- Stars