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Equation of state of stellar matter in a wide domain of thermodynamic parameters, characteristic for CCSN. From: T . Fischer, M . Hempel, I . Sagert, Y . Suwa, and J . Schaffner-Bielich , Eur. Phys. J. A (2014) 50: 46. Nuclear Statistical Equilibrium ( NSE).
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Equation of state of stellar matter in a wide domain of thermodynamic parameters, characteristic for CCSN
From: T. Fischer, M. Hempel, I. Sagert, Y. Suwa, and J. Schaffner-Bielich, Eur. Phys. J. A (2014) 50: 46
Nuclear Statistical Equilibrium (NSE) T9 3–4 (T9=T/109) i=(A,Z)
EoS under the conditions ofNSE 1,
The shock wave formation into a collapsing stellar core t = -0.9 ms t = 0.0 ms t = 10 ms t = 1.0 ms
Single nucleus approximation G. BAYM, H.A. BETHE, C.J. PETHICK Nuclear Physics A175 (1971) 225-27 1
Oyamatsu, Nuclear Physics A561 (1993) 431-452 S.B. R.uster, M. Hempel, and J. Schaffner-Bielich “The outer crust of non-accreting cold neutron stars”
S. Kreima, M. Hempel, D. Lunneyd, J. Schaffner-Bieliche “Nuclear Masses and Neutron Stars”
K. Oyamatsu, Nuclear Physics A 561 (1993) 431-452 C. J. Horowitz: Links Between Heavy Ion and Astrophysics
Pure uniform nuclear matter F.D. Swesty, J.M. Lattimer, E.S. Myra, Astroph. J. 425, 195-204 (1993) “Thermal properties of supernova matter: The bulk homogeneous phase” C. Constantinou, B. Muccioli,M. Prakash,J. M. Lattimer
From: T. Fischer, M. Hempel, I. Sagert, Y. Suwa, and J. Schaffner-Bielich, Eur. Phys. J. A (2014) 50: 46
Equation of state of dense matter The ravine of instability Sly EOS; Douchin & Haensel (2001)
Neutrino-matter interaction rates and neutrino transport
Kνи Sν– the energy and impulse fluxes, Uν– energy density of neutrinos, andμ–cosine of the angle between radius-vector and the neutrino direction.
A. Burrows, T.A. Thompson NEUTRINO-MATTER INTERACTION RATESIN SUPERNOVAE
S.W. Bruenn Astroph. J. Suppl. S., 58:771-841 (1985)
Oscillations C. Lunardinia, I. Tamborra “Difuse supernova neutrinos:oscillation eects, stellar cooling and progenitor mass dependence Kotake et al 2006