## NSR Query Results
Output year order : Descending NSR database version of May 24, 2024. Search: Author = M.R.Wu Found 8 matches.
Y.An, M.-R.Wu, G.Guo, Y.-L.Sming Tsai, Sh.-J.Huang, Y.-Zh.Fan
T.Fischer, G.Guo, A.A.Dzhioev, G.Martinez-Pinedo, M.-R.Wu, A.Lohs, Y.-Z.Qian
NUCLEAR REACTIONS
S.A.Giuliani, G.Martinez-Pinedo, M.-R.Wu, L.M.Robledo
NUCLEAR STRUCTURE Z=85-120, N=120-250; calculated highest fission barriers, energy windows for β-delayed fission and neutron-induced fission. A=100-240; A=180-350; Z=30-100, N=65-230; calculated abundances as function of mass number and neutron numbers. A=254, Z=89-99; calculated neutron-induced fission and neutron capture stellar reaction rates at 0.64 GK. A=220-230; calculated abundances, radioactive energy emitted by β and α decays, and fission as a function of time for different ejecta conditions, ejecta heating rate as a function of time. Finite range droplet model with Thomas-Fermi (FRDM+TF), Skyrme HFB14, and Barcelona-Catania-Paris-Madrid (BCPM), energy density functional (EDF) methods.
M.-R.Wu, J.Barnes, G.Martinez-Pinedo, B.D.Metzger
RADIOACTIVITY
S.A.Giuliani, G.Martinez-Pinedo, L.M.Robledo, M.-R.Wu
NUCLEAR REACTIONS Z=84-120(n, f), E not given; calculated fission rates, r-process abundances using TALYS code with BCPM EDF (Barcelona-Catania-Paris-Madrid Energy Density functional) and using Panov rates, r-process abundances. Compared with Solar abundances. RADIOACTIVITY Z=84-120(SF); calculated fission rates, r-process abundances using TALYS code with BCPM EDF (Barcelona-Catania-Paris-Madrid Energy Density functional) and using Panov rates, r-process abundances. Compared with Solar abundances.
T.Marketin, A.Sieverding, M.-R.Wu, N.Paar, G.Martinez-Pinedo
COMPILATION Z=8-110; compiled contribution of first-forbidden β-decay of neutron-rich nuclei to their total β-decay rate, T
RADIOACTIVITY Z=8-110(β
R.Knobel, M.Diwisch, F.Bosch, D.Boutin, L.Chen, C.Dimopoulou, A.Dolinskii, B.Franczak, B.Franzke, H.Geissel, M.Hausmann, C.Kozhuharov, J.Kurcewicz, S.A.Litvinov, G.Martinez-Pinedo, M.Matos, M.Mazzocco, G.Munzenberg, S.Nakajima, C.Nociforo, F.Nolden, T.Ohtsubo, A.Ozawa, Z.Patyk, W.R.Plass, C.Scheidenberger, J.Stadlmann, M.Steck, B.Sun, T.Suzuki, P.M.Walker, H.Weick, M.-R.Wu, M.Winkler, T.Yamaguchi
ATOMIC MASSES
J.Mendoza-Temis, M.-R.Wu, K.Langanke, G.Martinez-Pinedo, A.Bauswein, H.-T.Janka
ATOMIC MASSES A=108-288; calculated r-process abundances of slow ejecta for different mass models at different phases of the evolution in neutron star mergers using three-dimensional relativistic smoothed particle hydrodynamic simulation, and extended nuclear network of 7300 nuclei from free nucleons up to
NUCLEAR REACTIONS
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