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NSR database version of April 26, 2024.

Search: Author = I.Sultana

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2022SA20      Phys.Lett. B 829, 137059 (2022)

M.Saxena, W.-J.Ong, Z.Meisel, D.E.M.Hoff, N.Smirnova, P.C.Bender, S.P.Burcher, M.P.Carpenter, J.J.Carroll, A.Chester, C.J.Chiara, R.Conaway, P.A.Copp, B.P.Crider, J.Derkin, A.Estrae, G.Hamad, J.T.Harke, R.Jain, H.Jayatissa, S.N.Liddick, B.Longfellow, M.Mogannam, F.Montes, N.Nepal, T.H.Ogunbeku, A.L.Richard, H.Schatz, D.Soltesz, S.K.Subedi, I.Sultana, A.S.Tamashiro, V.Tripathi, Y.Xiao, R.Zink

⁵⁷Zn β-delayed proton emission establishes the ⁵⁶Ni rp-process waiting point bypass

RADIOACTIVITY ⁵⁷Zn(β⁺p), (β⁺) [from ⁹Be(⁷⁸Kr, X)⁵⁷Zn, E=150 MeV/nucleon]; measured decay products, Eγ, Iγ, Eβ, Iβ, Ep, Ip; deduced T_1/2, βp branching ratio, β-γ-p decay mode transitions. The Coupled Cyclotron Facility of NSCL.

doi: 10.1016/j.physletb.2022.137059
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Data from this article have been entered in the XUNDL database. For more information, click here.

2022SC17      J.Phys.(London) G49, 110502 (2022)

H.Schatz, A.D.Becerril Reyes, A.Best, E.F.Brown, K.Chatziioannou, K.A.Chipps, C.M.Deibel, R.Ezzeddine, D.K.Galloway, C.J.Hansen, F.Herwig, A.P.Ji, M.Lugaro, Z.Meisel, D.Norman, J.S.Read, L.F.Roberts, A.Spyrou, I.Tews, F.X.Timmes, C.Travaglio, N.Vassh, C.Abia, P.Adsley, S.Agarwal, M.Aliotta, W.Aoki, A.Arcones, A.Aryan, A.Bandyopadhyay, A.Banu, D.W.Bardayan, J.Barnes, A.Bauswein, T.C.Beers, J.Bishop, T.Boztepe, B.Cote, M.E.Caplan, A.E.Champagne, J.A.Clark, M.Couder, A.Couture, S.E.de Mink, S.Debnath, R.J.deBoer, J.den Hartogh, P.Denissenkov, V.Dexheimer, I.Dillmann, J.E.Escher, M.A.Famiano, R.Farmer, R.Fisher, C.Frohlich, A.Frebel, C.Fryer, G.Fuller, A.K.Ganguly, S.Ghosh, B.K.Gibson, T.Gorda, K.N.Gourgouliatos, V.Graber, M.Gupta, W.C.Haxton, A.Heger, W.R.Hix, W.C.G.Ho, E.M.Holmbeck, A.A.Hood, S.Huth, G.Imbriani, R.G.Izzard, R.Jain, H.Jayatissa, Z.Johnston, T.Kajino, A.Kankainen, G.G.Kiss, A.Kwiatkowski, M.La Cognata, A.M.Laird, L.Lamia, P.Landry, E.Laplace, K.D.Launey, D.Leahy, G.Leckenby, A.Lennarz, B.Longfellow, A.E.Lovell, W.G.Lynch, S.M.Lyons, K.Maeda, E.Masha, C.Matei, J.Merc, B.Messer, F.Montes, A.Mukherjee, M.R.Mumpower, D.Neto, B.Nevins, W.G.Newton, L.Q.Nguyen, K.Nishikawa, N.Nishimura, F.M.Nunes, E.O'Connor, B.W.O'Shea, W.-J.Ong, S.D.Pain, M.A.Pajkos, M.Pignatari, R.G.Pizzone, V.M.Placco, T.Plewa, B.Pritychenko, A.Psaltis, D.Puentes, Y.-Z.Qian, D.Radice, D.Rapagnani, B.M.Rebeiro, R.Reifarth, A.L.Richard, N.Rijal, I.U.Roederer, J.S.Rojo, J.S K, Y.Saito, A.Schwenk, M.L.Sergi, R.S.Sidhu, A.Simon, T.Sivarani, A.Skuladottir, M.S.Smith, A.Spiridon, T.M.Sprouse, S.Starrfield, A.W.Steiner, F.Strieder, I.Sultana, R.Surman, T.Szucs, A.Tawfik, F.Thielemann, L.Trache, R.Trappitsch, M.B.Tsang, A.Tumino, S.Upadhyayula, J.O.Valle Martinez, M.Van der Swaelmen, C.Viscasillas Vazquez, A.Watts, B.Wehmeyer, M.Wiescher, C.Wrede, J.Yoon, R.G.T.Zegers, M.A.Zermane, M.Zingale, the Horizon 2020 Collaborations

Horizons: nuclear astrophysics in the 2020s and beyond

doi: https://dx.doi.org/10.1088/1361-6471/ac8890
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2020GA12      Phys.Rev. C 101, 055805 (2020)

P.Gastis, G.Perdikakis, J.Dissanayake, P.Tsintari, I.Sultana, C.R.Brune, T.N.Massey, Z.Meisel, A.V.Voinov, K.Brandenburg, T.Danley, R.Giri, Y.Jones-Alberty, S.Paneru, D.Soltesz, S.Subedi

Constraining the destruction rate of ⁴⁰K in stellar nucleosynthesis through the study of the ⁴⁰Ar(p, n)⁴⁰K reaction

NUCLEAR REACTIONS ⁴⁰Ar(p, n)⁴⁰K, E(cm)=3.3-3.9 MeV; measured In, Eγ, Iγ, and differential σ(θ, E) using neutron time-of-flight technique with plastic scintillators for neutron detection and LaBr₃ scintillator for γ detection at the Edwards Accelerator Laboratory of Ohio University; deduced total σ(E), and partial σ(E) populating discrete states. ⁴⁰K(n, p), E(cm)=3.3-3.9 MeV; deduced thermonuclear reaction rates for the forward and reverse reactions. Comparison with Hauser-Feshbach calculations using the statistical model code TALYS, and with theoretical rates in the REACLIB library. Relevance to yield of ⁴⁰K in nucleosynthesis, and impact on galactic chemical evolution models for the study of properties of exoplanets.

doi: 10.1103/PhysRevC.101.055805
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Data from this article have been entered in the EXFOR database. For more information, access X4 datasetC2570.