Asymmetric Neutrino Reaction in Magnetized Proto-Neutron Stars in fully Relativistic Approach

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Nuclear Matter RMF Approach Different Mean-Field for p, n & Fermi Motion, Mom.Dep.-Spin Vector Magnetic-Field is treated perturbatively. Full Relativistic. Asymmetric Neutrino Reaction in Magnetized Proto-Neutron Stars in fully Relativistic Approach. ID-50. - PowerPoint PPT Presentation


Asymmetric Neutrino Reaction in Magnetized Proto-Neutron Stars in fully Relativistic Approach Magnetic Field increases neutrinos emitted in the direction parallel to the magnetic fieldand decreases that in its opposite direction T. Maruyama, T. Kajino, N. Yasutake, M.-K. Cheoun, C.-Y. RyuID-50r-process nucleosynthesis during the MHD explosions of a massive starThe origin of heavy neutron-rich elements like uraniumThe 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 3rd peak elements appear needs strong differential rotation and concentrated magnetic field.3rd peak can be reprocuced but the 2nd peak is low.52M.Saruwatari , M. Hashimoto (Kyusyu University), K. Kotake(NAOJ), S. Yamada(Waseda University)Effects of a new triple-alpha reaction rate on the helium ignition of accreting white dwarfsTriple (3) reaction plays an important role for the helium burning stage Recently, 3 reaction is calculated by Ogata et al (OKK).We investigate the effects of a newly calculated triple- 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.53M.Saruwatari , M. Hashimoto, R. Nakamura(Kyushu University)S. Fujimoto (Kumamoto National College of Technology), K. Arai(Kumamoto University)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 810, 2010ID 54We investigate the nucleosynthesis of a massive star at the stage of from hydrostatic evolution to its 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.Supernova neutrino The g-ray production in neutral-current O(n,n)XRCNP E148 16O(p,2p)15N*Proposed experiment to measure g-rays in O(p,p)X (DT=0,1) and O(3He,t)X(DT=1) ID-55The core-cusp problem in CDM halos and supernova feedbackGo Ogiya, Masao Mori (Univ. of Tsukuba, Japan)Navarro et al.(1997)log(r) [kpc]log() [10-10M kpc-3]log() [ M pc-3] -2 - 1 0 1 log(r) [kpc]Swaters et al. (2003)CuspCoreCDM simulationObservationNo. 59Result of N-body simulationN=1048576Cusp to Core transformationDeep potentialShallowpotentialGravitational field varianceThe 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.ID-60High-resolution Study of 56Fe 56Mn 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. ThiesEx (MeV)56Fe(3He, t)56Fe, =0 56Fe(p, p)56Fe, =3.5 1 : 12.5 : 1ID-62*