TABULATED EQUATION OF STATE FOR SUPERNOVA MATTER INCLUDING FULL NUCLEAR ENSEMBLE

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dc.contributor.authorBuyukcizmeci, N.
dc.contributor.authorBotvina, A. S.
dc.contributor.authorMishustin, I. N.
dc.date.accessioned2020-03-26T18:58:34Z
dc.date.available2020-03-26T18:58:34Z
dc.date.issued2014
dc.departmentSelçuk Üniversitesien_US
dc.description.abstractThis is an introduction to the tabulated database of stellar matter properties calculated within the framework of the Statistical Model for Supernova Matter (SMSM). The tables present thermodynamical characteristics and nuclear abundances for 31 values of baryon density (10(-8) < rho/rho(0) < 0.32, rho(0) = 0.15 fm(-3) is the normal nuclear matter density), 35 values of temperature (0.2MeV < T < 25 MeV), and 28 values of electron-to-baryon ratio (0.02 < Y-e < 0.56). The properties of stellar matter in beta equilibrium are also considered. The main ingredients of the SMSM are briefly outlined, and the data structure and content of the tables are explained.en_US
dc.description.sponsorshipFrankfurt Institute for Advanced Studies (FIAS); Helmholtz International Center for FAIR within the LOEWE program; Selcuk University-Scientific Research Projects (BAP)Selcuk University; EUEuropean Union (EU); [NSH-932.2014.2]en_US
dc.description.sponsorshipN.B. and A. S. B. are grateful to the Frankfurt Institute for Advanced Studies (FIAS) for support and hospitality. This work is supported by the Helmholtz International Center for FAIR within the LOEWE program. N.B. thanks the Selcuk University-Scientific Research Projects (BAP) for partial support. N.B. acknowledges that a part of the numerical calculations was carried out on the computers at the Physics Department of Selcuk University. N.B. is grateful to R. Ogul for encouragement and to A. E. Kavruk and T. Ozturk for help in computing. A. S. B. acknowledges support from the Research Infrastructure Integrating Activity "Study of Strongly Interacting Matter" Hadron-Physics3 under the 7th Framework Programme of EU. I.N.M. acknowledges support from grant NSH-932.2014.2 (Russia).en_US
dc.identifier.doi10.1088/0004-637X/789/1/33en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.issn1538-4357en_US
dc.identifier.issue1en_US
dc.identifier.scopusqualityQ1en_US
dc.identifier.urihttps://dx.doi.org/10.1088/0004-637X/789/1/33
dc.identifier.urihttps://hdl.handle.net/20.500.12395/31175
dc.identifier.volume789en_US
dc.identifier.wosWOS:000338103400033en_US
dc.identifier.wosqualityQ1en_US
dc.indekslendigikaynakWeb of Scienceen_US
dc.indekslendigikaynakScopusen_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.relation.ispartofASTROPHYSICAL JOURNALen_US
dc.relation.publicationcategoryMakale - Uluslararası Hakemli Dergi - Kurum Öğretim Elemanıen_US
dc.rightsinfo:eu-repo/semantics/openAccessen_US
dc.selcuk20240510_oaigen_US
dc.subjectdense matteren_US
dc.subjectequation of stateen_US
dc.subjectnuclear reactions, nucleosynthesis, abundancesen_US
dc.subjectstars: neutronen_US
dc.subjectsupernovae: generalen_US
dc.titleTABULATED EQUATION OF STATE FOR SUPERNOVA MATTER INCLUDING FULL NUCLEAR ENSEMBLEen_US
dc.typeArticleen_US

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