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.
N1 - Funding Information:
& Weaver 15& model), we calculated neutrino conversion probabilities as functions of neutrino energy taking account of the matter effects and studied how our original neutrino spectra change. As for the parameters of neutrino oscillation, we adopt Am& = 4.5. 10e5eV2, Am& = 3.2. 10-3eV2, sin’ 2& = 0.82, sin2 2eZ3 = 1.0, sin2 2e13 = 8.0. 10e4, most of which are values indicated by observations of solar and atmospheric neutrinos. We consider both the normal mass hierarchy and the inverted mass hierarchy. Our results are as follows. Average energies of time integrated neutrino spectra for the first 1Osecw ere originally 8.9MeV, 10.8MeV and 11.7MeV for v,, &, and V~ respectively without neutrino oscillation. With neutrino oscillation in the normal mass hierarchy, they become 11.7MeV, ll.lMeV, and 10.9MeV and in the inverted mass hierarchy, 10.8MeV, 11.7MeV, and 10.9MeV. As expected, average energies of v, and & increase due to the neutrino oscillation, but the increment is small because our original models without neutrino oscillation have small differences of mean energy between Y,/Y, and vIL. Although our simulations correspond only to the second half of supernova neutrinos, our models are consistent with observed SN1987A data [6,7] both in the cases with and without neutrino oscillation. Several authors [8,9] pointed out the possible inconsistency between the observed ve energy and large mixing models assuming high average energy of I,. As studied recently by Keil et al.[lO], we should investigate the emergent neutrino spectra in detail before putting strong constraints on neutrino oscillation parameters using observational data of supernova neutrinos. This work is in part supported by JSPS under the Grants-in-Aid Program for Scientific Research (12047230, 14039210) of the Ministry of Education, Science, Sports, and Culture of Japan, by RIKEN and by KEK Supercomputer Project No. 01-75 and 02-87.
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.
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U2 - 10.1016/S0375-9474(03)00894-7
DO - 10.1016/S0375-9474(03)00894-7
M3 - Article
AN - SCOPUS:0038586368
VL - 723
SP - 703c-705c
JO - Nuclear Physics A
JF - Nuclear Physics A
SN - 0375-9474
IS - 1-2
ER -