Stellar collapse with hadron-quark phase transition of hot and dense matter

Ken'ichiro Nakazato, Kohsuke Sumiyoshi, Shoichi Yamada

    Research output: Contribution to journalArticle

    Abstract

    We construct an equation of state (EOS) including the hadron-quark phase transition by the Gibbs conditions for finite temperature. We adopt the EOS based on the relativistic mean field theory for the hadronic phase and the MIT bag model of the deconfined 3-flavor strange quark matter for the quark phase. Moreover, the gravitational collapse of massive stars with several masses is computed using our EOS and we find that the phase transition makes the interval time from the bounce to the black hole formation, namely the duration time of the neutrino emission, shorter for the model with a bounce. This fact implies that we may be able to probe observationally the EOS of hot and dense matter in future.

    Original languageEnglish
    Pages (from-to)76-79
    Number of pages4
    JournalProgress of Theoretical Physics Supplement
    Issue number174
    Publication statusPublished - 2008

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    equations of state
    quarks
    gravitational collapse
    bags
    massive stars
    neutrinos
    intervals
    probes
    temperature

    ASJC Scopus subject areas

    • Physics and Astronomy (miscellaneous)

    Cite this

    Stellar collapse with hadron-quark phase transition of hot and dense matter. / Nakazato, Ken'ichiro; Sumiyoshi, Kohsuke; Yamada, Shoichi.

    In: Progress of Theoretical Physics Supplement, No. 174, 2008, p. 76-79.

    Research output: Contribution to journalArticle

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    AB - We construct an equation of state (EOS) including the hadron-quark phase transition by the Gibbs conditions for finite temperature. We adopt the EOS based on the relativistic mean field theory for the hadronic phase and the MIT bag model of the deconfined 3-flavor strange quark matter for the quark phase. Moreover, the gravitational collapse of massive stars with several masses is computed using our EOS and we find that the phase transition makes the interval time from the bounce to the black hole formation, namely the duration time of the neutrino emission, shorter for the model with a bounce. This fact implies that we may be able to probe observationally the EOS of hot and dense matter in future.

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