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R -process Nucleosynthesis in Supernova Explosions

R -process Nucleosynthesis in Supernova Explosions. Ryohei Fukuda 1 , Motoaki Saruwatari 1 , Masa-aki Hashimoto 1 , Shin- ichiro Fujimoto 2 1 D epartment of Physics, Kyushu University, Fukuoka 2 Department of Electronic Control, Kumamoto National College of Technology, Kumamoto.

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R -process Nucleosynthesis in Supernova Explosions

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  1. R-process Nucleosynthesis in Supernova Explosions Ryohei Fukuda1, Motoaki Saruwatari1, Masa-aki Hashimoto1, Shin-ichiro Fujimoto2 1Department of Physics, Kyushu University, Fukuoka 2 Department of Electronic Control, Kumamoto National College of Technology, Kumamoto M. Saruwatari, M. Hashimoto, R. Fukuda and S. Fujimoto, “R-process Nucleosynthesis in MHD Jet Explosions of Core-Collapse Super-novae,” Journal of Astrophysics , vol.2013, Article ID 506146, 13pages, 2013

  2. Introduction • r-process • One of the mechanisms to produce the elements heavier than Fe • High entropy or low electron fraction Ye are needed.(Hoffman+1999) • r-abundance pattern of r-process rich low metallicity stars : consistent with the solar one • Sites : supernovae (e.g., Winteler+2012) or neutron star mergers (e.g., Korobkin+2012) Cowan & Sneden 2006

  3. Motivation • Nishimura et al. 2006 • Adiabatic explosion without neutrino effects • R-elements distribution is almost consistent with the solar system abundances. • Neutrino capture processes enhance Ye and reduce the production of r-elements? • Winteler et al. 2012 • 3D MHD simulation with neutrino effects • Abundant r-elements • Short simulation time • To confirm the possibility of the r-process in SNe, we performed 2D MHD simulation including neutrino effects with longer simulation time

  4. Methods • MHD simulation • ZEUS-2D code (Stone & Norman 1992) • ShenEoS (Shen et al. 1998) • presupernova model : 3.3 M8 He core (Hashimoto 1995) • 0 < r < 4000 km, 0 < θ < π/2 (300 (r )×30 (θ) grid) which covers the Fe core and inner part of Si-rich layer • Including neutrino effects (leakage scheme) • Nucleosynthesis calculation • ~4000 nuclear species • FRDM & ETFSI mass model

  5. Initial conditions and models cm, cm

  6. Results ergs Model 5 produces jet like explosion. Only third peak is reproduced.

  7. Summary • We performed 2D MHD simulation of magnetorotationally driven SNe with neutrino effects using the leakage scheme. • Strong jet-like explosions are obtained in model 5. • We calculate nucelosynthesis inside the ejecta including the r-process. • The third peak is reproduced by model 5. • Supernova explosions cannot be excluded as a site of the r-process.

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