Protoneutron star cooling with a new equation of state

H. Suzuki, H. Kogure, F. Tomioka, K. Sumiyoshi, S. Yamada, H. Shen

    Research output: Contribution to journalArticle

    2 Citations (Scopus)

    Abstract

    Using a new numerical EOS (equation of state) table calculated by Shen et d., we performed numerical simulations of protoneutron star cooling. The EOS is based on the relativistic mean field theory, and the parameters in its Lagrangian have been chosen to reproduce the experimental properties of both stable and unstable nuclei. Furthermore, the numerical table covers such a wide range of thermodynamical quantities (temperature, 0 ∼1OOMeV; electron fraction, 0 ∼ 0.56; density, 10 5.1 ∼ 10 15.4g/cc) that cooling simulations even for 50 seconds could be done without troubles. The quasistatic evolution of protoneutron stars was investigated in detail with a numerical code including neutrino transfer (MGFLD scheme). Dependencies both on EOS and on initial models and implications to the SN1987A constraint on neutrino oscillation models are discussed.

    Original languageEnglish
    JournalNuclear Physics A
    Volume723
    Issue number1-2
    DOIs
    Publication statusPublished - 2003 Jul 28

    Fingerprint

    equations of state
    cooling
    stars
    neutrinos
    simulation
    oscillations
    nuclei
    electrons
    temperature

    ASJC Scopus subject areas

    • Nuclear and High Energy Physics

    Cite this

    Protoneutron star cooling with a new equation of state. / Suzuki, H.; Kogure, H.; Tomioka, F.; Sumiyoshi, K.; Yamada, S.; Shen, H.

    In: Nuclear Physics A, Vol. 723, No. 1-2, 28.07.2003.

    Research output: Contribution to journalArticle

    Suzuki, H, Kogure, H, Tomioka, F, Sumiyoshi, K, Yamada, S & Shen, H 2003, 'Protoneutron star cooling with a new equation of state', Nuclear Physics A, vol. 723, no. 1-2. https://doi.org/10.1016/S0375-9474(03)00894-7
    Suzuki, H. ; Kogure, H. ; Tomioka, F. ; Sumiyoshi, K. ; Yamada, S. ; Shen, H. / Protoneutron star cooling with a new equation of state. In: Nuclear Physics A. 2003 ; Vol. 723, No. 1-2.
    @article{98540cb2e4ce4170a82d4ba23c88f844,
    title = "Protoneutron star cooling with a new equation of state",
    abstract = "Using a new numerical EOS (equation of state) table calculated by Shen et d., we performed numerical simulations of protoneutron star cooling. The EOS is based on the relativistic mean field theory, and the parameters in its Lagrangian have been chosen to reproduce the experimental properties of both stable and unstable nuclei. Furthermore, the numerical table covers such a wide range of thermodynamical quantities (temperature, 0 ∼1OOMeV; electron fraction, 0 ∼ 0.56; density, 10 5.1 ∼ 10 15.4g/cc) that cooling simulations even for 50 seconds could be done without troubles. The quasistatic evolution of protoneutron stars was investigated in detail with a numerical code including neutrino transfer (MGFLD scheme). Dependencies both on EOS and on initial models and implications to the SN1987A constraint on neutrino oscillation models are discussed.",
    author = "H. Suzuki and H. Kogure and F. Tomioka and K. Sumiyoshi and S. Yamada and H. Shen",
    year = "2003",
    month = "7",
    day = "28",
    doi = "10.1016/S0375-9474(03)00894-7",
    language = "English",
    volume = "723",
    journal = "Nuclear Physics A",
    issn = "0375-9474",
    publisher = "Elsevier",
    number = "1-2",

    }

    TY - JOUR

    T1 - Protoneutron star cooling with a new equation of state

    AU - Suzuki, H.

    AU - Kogure, H.

    AU - Tomioka, F.

    AU - Sumiyoshi, K.

    AU - Yamada, S.

    AU - Shen, H.

    PY - 2003/7/28

    Y1 - 2003/7/28

    N2 - Using a new numerical EOS (equation of state) table calculated by Shen et d., we performed numerical simulations of protoneutron star cooling. The EOS is based on the relativistic mean field theory, and the parameters in its Lagrangian have been chosen to reproduce the experimental properties of both stable and unstable nuclei. Furthermore, the numerical table covers such a wide range of thermodynamical quantities (temperature, 0 ∼1OOMeV; electron fraction, 0 ∼ 0.56; density, 10 5.1 ∼ 10 15.4g/cc) that cooling simulations even for 50 seconds could be done without troubles. The quasistatic evolution of protoneutron stars was investigated in detail with a numerical code including neutrino transfer (MGFLD scheme). Dependencies both on EOS and on initial models and implications to the SN1987A constraint on neutrino oscillation models are discussed.

    AB - Using a new numerical EOS (equation of state) table calculated by Shen et d., we performed numerical simulations of protoneutron star cooling. The EOS is based on the relativistic mean field theory, and the parameters in its Lagrangian have been chosen to reproduce the experimental properties of both stable and unstable nuclei. Furthermore, the numerical table covers such a wide range of thermodynamical quantities (temperature, 0 ∼1OOMeV; electron fraction, 0 ∼ 0.56; density, 10 5.1 ∼ 10 15.4g/cc) that cooling simulations even for 50 seconds could be done without troubles. The quasistatic evolution of protoneutron stars was investigated in detail with a numerical code including neutrino transfer (MGFLD scheme). Dependencies both on EOS and on initial models and implications to the SN1987A constraint on neutrino oscillation models are discussed.

    UR - http://www.scopus.com/inward/record.url?scp=0038586368&partnerID=8YFLogxK

    UR - http://www.scopus.com/inward/citedby.url?scp=0038586368&partnerID=8YFLogxK

    U2 - 10.1016/S0375-9474(03)00894-7

    DO - 10.1016/S0375-9474(03)00894-7

    M3 - Article

    AN - SCOPUS:0038586368

    VL - 723

    JO - Nuclear Physics A

    JF - Nuclear Physics A

    SN - 0375-9474

    IS - 1-2

    ER -