A comparative study of statistical models for nuclear equation of state of stellar matter

Basit Öğe Kaydı
dc.contributor.authorBuyukcizmeci, N.
dc.contributor.authorBotvina, A. S.
dc.contributor.authorMishustin, I. N.
dc.contributor.authorOgul, R.
dc.contributor.authorHempel, M.
dc.contributor.authorSchaffner-Bielich, J.
dc.contributor.authorThielemann, F. -K.
dc.date.accessioned2020-03-26T18:40:58Z
dc.date.available2020-03-26T18:40:58Z
dc.date.issued2013
dc.departmentSelçuk Üniversitesien_US
dc.description.abstractWe compare three different statistical models for the equation of state (EOS) of stellar matter at sub-nuclear densities and temperatures (0.5-10 MeV) expected to occur during the collapse of massive stars and supernova explosions. The models introduce the distributions of various nuclear species in nuclear statistical equilibrium, but use somewhat different nuclear physics inputs. It is demonstrated that the basic thermodynamical quantities of stellar matter under these conditions are similar, except in the region of high densities and low temperatures. We demonstrate that mass and isotopic distributions have considerable differences related to the different assumptions of the models on properties of nuclei at these stellar conditions. Overall, the three models give similar trends, but the details reflect the uncertainties related to the modeling of medium effects, such as the temperature and density dependence of surface and bulk energies of heavy nuclei, and the nuclear shell structure effects. We discuss importance of new physics inputs for astrophysical calculations from experimental data obtained in intermediate energy heavy-ion collisions, in particular, the similarities of the conditions reached during supernova explosions and multifragmentation reactions. (c) 2013 Elsevier B.V. All rights reserved.en_US
dc.description.sponsorshipHIC for FAIR (LOEWE program); Frankfurt Institute for Advanced Studies (FIAS); High Performance and High Productivity Computing Project [HP2C]; Swiss National Science Foundation (SNF)Swiss National Science Foundation (SNSF) [200020-132816/1]; German Research Foundation (DFG) within the framework of the excellence initiative through the Heidelberg Graduate School of Fundamental PhysicsGerman Research Foundation (DFG); HPCI Strategic Program from the Ministry of Education, Culture, Sports, Science and Technology (MEXT) in Japan; Japan Society for the Promotion of Science Research Fellowship for Young ScientistsMinistry of Education, Culture, Sports, Science and Technology, Japan (MEXT)Japan Society for the Promotion of Science [24E79]; CompStar; [NSH-215.2012.2]; [20105004]; [20105005]; [19104006]; [21540281]; [22540296]; [24244036]en_US
dc.description.sponsorshipN.B. and A.S.B. are supported by HIC for FAIR (LOEWE program) and grateful to Frankfurt Institute for Advanced Studies (FIAS) for support and hospitality. I.N.M. acknowledges partial support provided by grant NSH-215.2012.2 (Russia). M.H. is supported by the High Performance and High Productivity Computing Project (HP2C), and the Swiss National Science Foundation (SNF) under project No. 200020-132816/1. M.H. thanks Matthias Liebendorfer for useful discussions of the manuscript. J.S.-B. is supported by the German Research Foundation (DFG) within the framework of the excellence initiative through the Heidelberg Graduate School of Fundamental Physics. The authors are additionally supported by CompStar, a research networking program of the European Science Foundation (ESF). F.-K.T. and M.H. are also grateful for participating in the EuroGENESIS collaborative research program of the ESF and the ENSAR/THEXO project. K.S., H.S. and S.Y. are partially supported by the Grant-in-Aid for Scientific Research on Innovative Areas (Nos. 20105004, 20105005), the Grant-in-Aid for the Scientific Research (Nos. 19104006, 21540281, 22540296, 24244036) and the HPCI Strategic Program from the Ministry of Education, Culture, Sports, Science and Technology (MEXT) in Japan. S.F. is grateful to FIAS for generous support. S.F. is supported by the Japan Society for the Promotion of Science Research Fellowship for Young Scientists (24E79). A part of the numerical calculations were carried out on SR16000 at YITP in Kyoto University. K.S. acknowledges the usage of the super-computers at Research Center for Nuclear Physics (RCNP) in Osaka University, The University of Tokyo, Yukawa Institute for Theoretical Physics (YITP) in Kyoto University and High Energy Accelerator Research Organization (KEK). K.S. is grateful to the organizers of NUFRA2011, where this project was initiated, for fruitfully discussions and extensive collaborations afterwards.en_US
dc.identifier.doi10.1016/j.nuclphysa.2013.03.010en_US
dc.identifier.endpage54en_US
dc.identifier.issn0375-9474en_US
dc.identifier.issn1873-1554en_US
dc.identifier.scopusqualityQ2en_US
dc.identifier.startpage13en_US
dc.identifier.urihttps://dx.doi.org/10.1016/j.nuclphysa.2013.03.010
dc.identifier.urihttps://hdl.handle.net/20.500.12395/29139
dc.identifier.volume907en_US
dc.identifier.wosWOS:000320208400002en_US
dc.identifier.wosqualityQ2en_US
dc.indekslendigikaynakWeb of Scienceen_US
dc.indekslendigikaynakScopusen_US
dc.language.isoenen_US
dc.publisherELSEVIERen_US
dc.relation.ispartofNUCLEAR PHYSICS Aen_US
dc.relation.publicationcategoryMakale - Uluslararası Hakemli Dergi - Kurum Öğretim Elemanıen_US
dc.rightsinfo:eu-repo/semantics/closedAccessen_US
dc.selcuk20240510_oaigen_US
dc.subjectNuclear astrophysicsen_US
dc.titleA comparative study of statistical models for nuclear equation of state of stellar matteren_US
dc.typeArticleen_US

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