1. Asymmetric Neutrino Reaction in Magnetized Proto-Neutron Stars in fully Relativistic Approach Nuclear Matter ⇒ RMF Approach Different Mean-Field for p, n & Λ Fermi Motion, Mom.Dep.-Spin Vector Magnetic-Field is treated perturbatively Full Relativistic Magnetic Field increases neutrinos emitted in the direction parallel to the magnetic field and decreases that in its opposite direction T. Maruyama, T. Kajino, N. Yasutake, M.-K. Cheoun, C.-Y. Ryu ID-50

2. r-process nucleosynthesis during the MHD explosions of a massive star The origin of heavy neutron-rich elements like uranium The possibility of the r-process during the magnetohydrohynamical explosion of supernova in a massive star of 13 solar mass with the effects of neutrinos induced. Low Ye ejecta from which the 3 rd peak elements appear needs strong differential rotation and concentrated magnetic field. 3 rd peak can be reprocuced but the 2nd peak is low. 52 M.Saruwatari, M. Hashimoto (Kyusyu University), K. Kotake(NAOJ), S. Yamada(Waseda University)

3. Effects of a new triple-alpha reaction rate on the helium ignition of accreting white dwarfs Triple – α (3α) reaction plays an important role for the helium burning stage Recently, 3α reaction is calculated by Ogata et al (OKK). We investigate the effects of a newly calculated triple-α reaction rate (OKK rate) on the helium flashes. The helium ignitions occur in the low density by two orders of magnitude if the OKK rate is adopted. Nuclear flashes are triggered for all cases of A-F in the helium layers. 53 M.Saruwatari, M. Hashimoto, R. Nakamura(Kyushu University) S. Fujimoto (Kumamoto National College of Technology), K. Arai(Kumamoto University)

4. Heavy-element Nucleosynthesis in Magnetohydrodynamical Jets from Collapsars M. Ono, M. Hashimoto (Kyushu Univ.), S. Fujimoto (Kumamoto Nat. Coll. Tech.), K. Kotake (NAOJ), S. Yamada (Waseda Univ.) OMEG10 at RCNP, Osaka University, on March 8–10, 2010 ID 54 Y e > 0.45 only (464 nuclide up to 94 Kr) Total (4463 nuclide up to 292 Am) We investigate the nucleosynthesis of a massive star at the stage of from hydrostatic evolution to it’s jet-like supernova explosion driven by magnetohydrodynamical effects of differentially rotating core (Collapsar). Hydrostatic, explosive(464 nuclide), and heavy-element (4463 nuclide) nucleosyntheses are performed. Finally, all results are combined and compared with solar abundances.

5. T.Mori, M.Sakuda(Okayama), A.Tamii, H.Toki(RCNP), M.Nakahata, K.Ueno(ICRR) Study of  -ray production from - 16 O interactions and the detection of neutrinos from Supernova explosion Supernova neutrino The  -ray production in neutral-current O(  ’)X RCNP E148 16 O(p,2p) 15 N* Proposed experiment to measure  -rays in O(p,p’)X (  T=0,1) and O( 3 He,t)X(  T=1) Only Charged-Current events were considered in the previous SN search. But, a significant number of Neutral- Current  -ray production (E>5MeV) exist, which can be observed in the detector. Neutrino events from SN at 10kpc expected at Super-K. Ikeda et.al.APJ’07. CC events NC events Motivated by Ejiri’s s-hole idea on proton decay and NC -O interaction, E148 experiment O(p,2p)N* measured  -ray spectrum for E>5 MeV at RCNP. It measured the excitation energy (E x) and the  -ray energy (E  ). NaI NaI (E  ) target Excitation energy(MeV) We like to measure the  -rays in the energy E  =5-20MeV in O(p,p’)X (  T=0,1) and O( 3 He,t)X (  T=1) at RCNP, similar to E148 experiment. Thus, the  -rays associated with both Fermi and Gamov-Teller nuclear transitions can be systematically studied. 16 O(p,p’) Ref. T.Kawabata’s Ph.D.(2002) 16 O( 3 He,t)F Ref. H.Fujita et.al.,PRC79(‘09) NC  CC e ± NC  T=0 T=1 16 O  15 N+p 15 N* 15 O+n 15 O*   NC  production is estimated by Langanke et al.,PRL96,’96, based on the excitation of giant resonances. (, ’) Neutrino events ID-55

6. The core-cusp problem in CDM halos and supernova feedback Go Ogiya, Masao Mori (Univ. of Tsukuba, Japan) Navarro et al.(1997) log(r) [kpc] log(ρ) [10 -10 M ☉ kpc -3 ] log(ρ) [ M ☉ pc -3 ] -2 - 1 0 1 log(r) [kpc] Swaters et al. (2003) Cusp Core CDM simulationObservation No. 59 Result of N-body simulation N=1048576 Cusp to Core transformation SNe driven gas eject Deep potential Shallowpotential Gravitational field variance “The Core-Cusp problem” is an open question on CDM cosmology. We study about dynamical response of a CDM halo to mass loss driven by supernova feedback using N-body simulations. The dynamical evolution of the central density profile also depends on mass loss timescale. We discuss the relation among our model, the star formation rate and the metal enrichment.

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8. High-resolution Study of 56 Fe → 56 Mn Gamow-Teller Transition M. Nagashima, Y. Shimbara, H. Fujita, Y. Fujita, T. Adachi, N. T. Botha, E. Ganioglu, K. Hatanaka, N. T. Khai, K. Nakanishi, R. Neveling, H. Okamura, Y.Sakemi, Y. Shimizu, G. Susoy, T.Suzuki, A. Tamii, J. Thies E x (MeV) 56 Fe(n,p) 56 Mn, θ=0° M.C. Vetterli et. al., Phys. Rev. C 40, 559(1989) 56 Fe( 3 He, t) 56 Fe, θ=0° 56 Fe(p, p’) 56 Fe, θ=3.5° 1 : 1 2.5 : 1 ID-62