EOS of hyperonic matter for core-collapse supernovae

A. Ohnishi, K. Tsubakihara, K. Sumiyoshi, C. Ishizuka, Shoichi Yamada, H. Suzuki

    Research output: Contribution to journalArticle

    5 Citations (Scopus)

    Abstract

    We discuss the properties of the supernova matter equation of state (EOS) including hyperons, and the emergence of hyperons in dynamical core-collapse processes. The recently tabulated EOS including hyperons is based on an SUf (3) extended relativistic mean field (RMF) model, in which the coupling constants of hyperons with scalar mesons are determined to fit the hyperon potential depths in nuclear matter, (UΣ, UΞ) = (+ 30 MeV, - 15 MeV), which are suggested from recent analyses of hyperon production reactions. Hyperon effects are found to be small in the core-collapse and bounce stages, but abundant hyperons appear when the temperature becomes high during black hole formation and promote earlier collapse of the accreting proto-neutron star. The maximum mass of a hot proto-neutron star is discussed, and we give a rough estimate of the critical mass of the accreting proto-neutron star, at which the proto-neutron star re-collapses to a black hole.

    Original languageEnglish
    Pages (from-to)374-377
    Number of pages4
    JournalNuclear Physics A
    Volume835
    Issue number1-4
    DOIs
    Publication statusPublished - 2010 Apr 1

    Fingerprint

    hyperons
    supernovae
    equations of state
    neutron stars
    critical mass
    hot stars
    mesons
    scalars
    estimates

    Keywords

    • black hole
    • EOS
    • hyperon
    • neutrino
    • supernova

    ASJC Scopus subject areas

    • Nuclear and High Energy Physics

    Cite this

    Ohnishi, A., Tsubakihara, K., Sumiyoshi, K., Ishizuka, C., Yamada, S., & Suzuki, H. (2010). EOS of hyperonic matter for core-collapse supernovae. Nuclear Physics A, 835(1-4), 374-377. https://doi.org/10.1016/j.nuclphysa.2010.01.222

    EOS of hyperonic matter for core-collapse supernovae. / Ohnishi, A.; Tsubakihara, K.; Sumiyoshi, K.; Ishizuka, C.; Yamada, Shoichi; Suzuki, H.

    In: Nuclear Physics A, Vol. 835, No. 1-4, 01.04.2010, p. 374-377.

    Research output: Contribution to journalArticle

    Ohnishi, A, Tsubakihara, K, Sumiyoshi, K, Ishizuka, C, Yamada, S & Suzuki, H 2010, 'EOS of hyperonic matter for core-collapse supernovae', Nuclear Physics A, vol. 835, no. 1-4, pp. 374-377. https://doi.org/10.1016/j.nuclphysa.2010.01.222
    Ohnishi A, Tsubakihara K, Sumiyoshi K, Ishizuka C, Yamada S, Suzuki H. EOS of hyperonic matter for core-collapse supernovae. Nuclear Physics A. 2010 Apr 1;835(1-4):374-377. https://doi.org/10.1016/j.nuclphysa.2010.01.222
    Ohnishi, A. ; Tsubakihara, K. ; Sumiyoshi, K. ; Ishizuka, C. ; Yamada, Shoichi ; Suzuki, H. / EOS of hyperonic matter for core-collapse supernovae. In: Nuclear Physics A. 2010 ; Vol. 835, No. 1-4. pp. 374-377.
    @article{8a4806eb8ee04ceb9a3fa1be0917df19,
    title = "EOS of hyperonic matter for core-collapse supernovae",
    abstract = "We discuss the properties of the supernova matter equation of state (EOS) including hyperons, and the emergence of hyperons in dynamical core-collapse processes. The recently tabulated EOS including hyperons is based on an SUf (3) extended relativistic mean field (RMF) model, in which the coupling constants of hyperons with scalar mesons are determined to fit the hyperon potential depths in nuclear matter, (UΣ, UΞ) = (+ 30 MeV, - 15 MeV), which are suggested from recent analyses of hyperon production reactions. Hyperon effects are found to be small in the core-collapse and bounce stages, but abundant hyperons appear when the temperature becomes high during black hole formation and promote earlier collapse of the accreting proto-neutron star. The maximum mass of a hot proto-neutron star is discussed, and we give a rough estimate of the critical mass of the accreting proto-neutron star, at which the proto-neutron star re-collapses to a black hole.",
    keywords = "black hole, EOS, hyperon, neutrino, supernova",
    author = "A. Ohnishi and K. Tsubakihara and K. Sumiyoshi and C. Ishizuka and Shoichi Yamada and H. Suzuki",
    year = "2010",
    month = "4",
    day = "1",
    doi = "10.1016/j.nuclphysa.2010.01.222",
    language = "English",
    volume = "835",
    pages = "374--377",
    journal = "Nuclear Physics A",
    issn = "0375-9474",
    publisher = "Elsevier",
    number = "1-4",

    }

    TY - JOUR

    T1 - EOS of hyperonic matter for core-collapse supernovae

    AU - Ohnishi, A.

    AU - Tsubakihara, K.

    AU - Sumiyoshi, K.

    AU - Ishizuka, C.

    AU - Yamada, Shoichi

    AU - Suzuki, H.

    PY - 2010/4/1

    Y1 - 2010/4/1

    N2 - We discuss the properties of the supernova matter equation of state (EOS) including hyperons, and the emergence of hyperons in dynamical core-collapse processes. The recently tabulated EOS including hyperons is based on an SUf (3) extended relativistic mean field (RMF) model, in which the coupling constants of hyperons with scalar mesons are determined to fit the hyperon potential depths in nuclear matter, (UΣ, UΞ) = (+ 30 MeV, - 15 MeV), which are suggested from recent analyses of hyperon production reactions. Hyperon effects are found to be small in the core-collapse and bounce stages, but abundant hyperons appear when the temperature becomes high during black hole formation and promote earlier collapse of the accreting proto-neutron star. The maximum mass of a hot proto-neutron star is discussed, and we give a rough estimate of the critical mass of the accreting proto-neutron star, at which the proto-neutron star re-collapses to a black hole.

    AB - We discuss the properties of the supernova matter equation of state (EOS) including hyperons, and the emergence of hyperons in dynamical core-collapse processes. The recently tabulated EOS including hyperons is based on an SUf (3) extended relativistic mean field (RMF) model, in which the coupling constants of hyperons with scalar mesons are determined to fit the hyperon potential depths in nuclear matter, (UΣ, UΞ) = (+ 30 MeV, - 15 MeV), which are suggested from recent analyses of hyperon production reactions. Hyperon effects are found to be small in the core-collapse and bounce stages, but abundant hyperons appear when the temperature becomes high during black hole formation and promote earlier collapse of the accreting proto-neutron star. The maximum mass of a hot proto-neutron star is discussed, and we give a rough estimate of the critical mass of the accreting proto-neutron star, at which the proto-neutron star re-collapses to a black hole.

    KW - black hole

    KW - EOS

    KW - hyperon

    KW - neutrino

    KW - supernova

    UR - http://www.scopus.com/inward/record.url?scp=77649286788&partnerID=8YFLogxK

    UR - http://www.scopus.com/inward/citedby.url?scp=77649286788&partnerID=8YFLogxK

    U2 - 10.1016/j.nuclphysa.2010.01.222

    DO - 10.1016/j.nuclphysa.2010.01.222

    M3 - Article

    AN - SCOPUS:77649286788

    VL - 835

    SP - 374

    EP - 377

    JO - Nuclear Physics A

    JF - Nuclear Physics A

    SN - 0375-9474

    IS - 1-4

    ER -