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Equations of state for hot neutron stars

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Abstract

We review the equation of state (EoS) models covering a large range of temperatures, baryon number densities and electron fractions presently available on the CompOSE database. These models are intended to be directly usable within numerical simulations of core-collapse supernovae, binary neutron star mergers and proto-neutron star evolution. We discuss their compliance with existing constraints from astrophysical observations and nuclear data. For a selection of purely nucleonic models in reasonable agreement with the above constraints, after discussing the properties of cold matter, we review thermal properties for thermodynamic conditions relevant for core-collapse supernovae and binary neutron star mergers. We find that the latter are strongly influenced by the density dependence of the nucleon effective mass. The selected bunch of models is used to investigate the EoS dependence of hot star properties, where entropy per baryon and electron fraction profiles are inspired from proto-neutron star evolution. The \(\varGamma \)-law analytical thermal EoS used in many simulations is found not to describe well these thermal properties of the EoS. However, it may offer a fair description of the structure of hot stars whenever thermal effects on the baryonic part are small, as shown here for proto-neutron stars starting from several seconds after bounce.

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Notes

  1. As of August, 30, 2021.

  2. https://compose.obspm.fr/.

  3. The TNTYST table on CompOSE does not provide that data, see Fig. 9 in [91] for that model.

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Acknowledgements

The authors gratefully acknowledge discussions with Fiorella Burgio and Stefan Typel. We thank Aurélien Pascal for providing us with the profiles in Fig. 25. We also thank the anonymous referee for constructive comments that significantly contributed to enhancing the manuscript’s quality. A.R.R. and F.N. acknowledge support from a grant of the Ministry of Research, Innovation and Digitization, CNCS/CCCDI-UEFISCDI, Project No. PN-III-P4-ID-PCE-2020-0293, within PNCDI III. This work has been partially funded by the European COST Action CA16214 PHAROS “The multi-messenger physics and astrophysics of neutron stars”.

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Authors and Affiliations

  1. National Institute for Physics and Nuclear Engineering (IFIN-HH), 077125, Bucharest, Romania

    Adriana R. Raduta & Flavia Nacu

  2. LUTH, Observatoire de Paris, Université PSL, CNRS, Université de Paris, 92190, Meudon, France

    Micaela Oertel

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  1. Adriana R. Raduta
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  2. Flavia Nacu
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Correspondence to Adriana R. Raduta.

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Communicated by Laura Tolos.

Appendix A

Appendix A

See Fig. 27.

Fig. 27
figure 27

Matter composition in terms of particle mass fractions and average mass and charge numbers of nuclei as predicted by HS(DD2), GRDF1(DD2) and GRDF2(DD2) for T=5 MeV (first two columns) and T=9 MeV (columns 3 and 4) and \(Y_e=0.5\)

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Raduta, A.R., Nacu, F. & Oertel, M. Equations of state for hot neutron stars. Eur. Phys. J. A 57, 329 (2021). https://doi.org/10.1140/epja/s10050-021-00628-z

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