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 language | English |
|---|---|
| Journal | Nuclear Physics A |
| Volume | 723 |
| Issue number | 1-2 |
| DOIs | |
| Publication status | Published - 2003 Jul 28 |
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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 journal › Article
}
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 -