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Neutrino reactions on two-nucleon system and core-collapse supernova

Neutrino reactions on two-nucleon system and core-collapse supernova. Shota Nasu ( Osaka.U ) Collaborators: T . Sato ( Osaka.U ), K. Sumiyoshi (Numazu Coll.Tech . ), S. Nakamura ( JLab ), F. Myhrer (USC), K.Kubodera (USC). Introduction : neutrino reactions in core-collapse supernovae.

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Neutrino reactions on two-nucleon system and core-collapse supernova

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  1. Neutrino reactions on two-nucleon system and core-collapse supernova ShotaNasu(Osaka.U) Collaborators: T. Sato(Osaka.U),K. Sumiyoshi(Numazu Coll.Tech.), S. Nakamura (JLab),F. Myhrer (USC),K.Kubodera(USC)

  2. Introduction: neutrino reactions in core-collapse supernovae Absorption, production and scattering reactions Electron capturesElastic scattering Pair creation and annihilation Nucleon Bremsstrahlung S. Bruenn (1985) Neutrino absorption:heating mechanism (shock wave revival -> delayed explosion) production:cooling mechanism (proto-neutron star to neutron star, source of neutrinos) Existence of light elements (d,t,3He) A. Arcones et al. (2008) K. Sumiyoshi and G.Röpke, (2008) • Neutrino absorption reaction in light elements ( for heating ) : S. X. Nakamura et al.(2009) : E. O’Connor et al., (2007), A. Arcones et al., (2008) In this work: neutrino productionreactionin two-nucleon system (forcooling)

  3. Motivation: Neutrino production in two nucleon collision Modified URCA processes : Neutrino bremsstrahlung : Crucial for cooling mechanism Friman and Maxwell (1979) One-pion-exchange Hanhaltet al.(2001) Low Energy Theorem deuteron in final state : EFT: deuteron as dibaryon Ando, Kubodera (2006) Those works can be used only low energy region. Objective : Analysis of neutrino production reactions on two-nucleon system for SN simulations Today’s talk : process

  4. Formalism Weak Hamiltonian: Standard Nuclear Physics Approach (SNPA) Nuclear currents: exchange currents + excited exchange currents model of nuclear current used to analyze nu-d for SNO data

  5. Neutrino emissivity Charged current process S.W.Bruenn(1985) T.A.Thompson et al.(2000)etc. : emitted neutrino energy : Fermi-Dirac distribution function

  6. emissivity for nucleon non-degenerate limit for lepton Examine the simple case : n-n kinetic energy → keep only dominant 1S0(nn) -> 3S1(d) Gamov-Teller transition : Neutron density Strong E-dependence of |M|  large 1S0 scattering length Energy dependence of Even at low temperature.. The facter enhances the high energy contribution

  7. Full result of emissivity IA+EXC nuclear currents, Including higher partial waves OPE model, approx. E-independent |M| T.A.Thompson et al. (2000) etc.

  8. Summary Analysis of neutrino emissivity near future plan ・ examine validity of using low energy approximation ・complete table of whole reactions rates including electron capture

  9. 150ms after core bounce t d shock position

  10. B: deuteron binding energy : neutron mass fraction : mass density in units of

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