TY - JOUR
T1 - Reduction of neutrino-nucleon scattering rate by nucleon-nucleon collisions
AU - Yamada, Shoichi
N1 - Funding Information:
I gratefully acknowledge critical discussions with H.-Th. Janka, G. Raffelt and H. Toki. I would highly appreciate various support by E. Müller during the stay in Max Planck Institut für Astrophysik. This work is partially supported by the Japanese Society for the Promotion of Science (JSPS), Postdoctoral Fellowships for Research Abroad and by the Grants-in-Aid for the Center-of-Excellence (COE) Research of the Ministry of Education, Science, Sports and Culture of Japan to RESCEU (No.07CE2002).
PY - 2000/1/3
Y1 - 2000/1/3
N2 - We studied possible modifications of the neutrino-nucleon scattering rate due to the nucleon-nucleon collisions in the hot dense matter which we find in the supernova core. We show that the finite width of the nucleon spectral function induced by the nucleon collisions leads to a broadening of the dynamical spin structure function of the nucleon, resulting in a reduction of the rate of neutrino-nucleon scattering via the axial vector current and making the energy exchange between neutrinos and nucleons easier. The reduction rate is relatively large, ∼ 0.6, even at density ∼ 1013g/cm3 and could have a significant impact on the dynamics of the collapse-driven supernova as well as the cooling of the proto neutron star.
AB - We studied possible modifications of the neutrino-nucleon scattering rate due to the nucleon-nucleon collisions in the hot dense matter which we find in the supernova core. We show that the finite width of the nucleon spectral function induced by the nucleon collisions leads to a broadening of the dynamical spin structure function of the nucleon, resulting in a reduction of the rate of neutrino-nucleon scattering via the axial vector current and making the energy exchange between neutrinos and nucleons easier. The reduction rate is relatively large, ∼ 0.6, even at density ∼ 1013g/cm3 and could have a significant impact on the dynamics of the collapse-driven supernova as well as the cooling of the proto neutron star.
UR - http://www.scopus.com/inward/record.url?scp=0034598210&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=0034598210&partnerID=8YFLogxK
U2 - 10.1016/S0375-9474(99)00429-7
DO - 10.1016/S0375-9474(99)00429-7
M3 - Article
AN - SCOPUS:0034598210
SN - 0375-9474
VL - 662
SP - 219
EP - 232
JO - Nuclear Physics A
JF - Nuclear Physics A
IS - 1-2
ER -