Neutron-star-merger equation of state

  • In this work, we discuss the dense matter equation of state (EOS) for the extreme range of conditions encountered in neutron stars and their mergers. The calculation of the properties of such an EOS involves modeling different degrees of freedom (such as nuclei, nucleons, hyperons, and quarks), taking into account different symmetries, and including finite density and temperature effects in a thermodynamically consistent manner. We begin by addressing subnuclear matter consisting of nucleons and a small admixture of light nuclei in the context of the excluded volume approach. We then turn our attention to supranuclear homogeneous matter as described by the Chiral Mean Field (CMF) formalism. Finally, we present results from realistic neutron-star-merger simulations performed using the CMF model that predict signatures for deconfinement to quark matter in gravitational wave signals.

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Author:Verônica Antocheviz DexheimerORCiDGND, Constantinos Constantinou, Elias Roland MostORCiDGND, Ludwig Jens PapenfortORCiD, Matthias HanauskeGND, Stefan SchrammGND, Horst StöckerORCiDGND, Luciano RezzollaORCiDGND
Parent Title (German):Universe
Place of publication:Basel
Document Type:Article
Date of Publication (online):2019/05/25
Date of first Publication:2019/05/25
Publishing Institution:Universitätsbibliothek Johann Christian Senckenberg
Release Date:2020/04/30
Tag:gravitational wave; neutron-star-merger; quark matter
Page Number:9
This is an open access article distributed under the Creative Commons Attribution License which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
Institutes:Physik / Physik
Wissenschaftliche Zentren und koordinierte Programme / Frankfurt Institute for Advanced Studies (FIAS)
Dewey Decimal Classification:5 Naturwissenschaften und Mathematik / 53 Physik / 530 Physik
Licence (German):License LogoCreative Commons - Namensnennung 4.0