NSR Query Results
Output year order : Descending NSR database version of April 26, 2024. Search: Author = M.Pignatari Found 45 matches. 2023HO07 Astrophys.J. 950, 133 (2023) S.Q.Hou, J.B.Liu, T.C.L.Trueman, J.G.Li, M.Pignatari, C.A.Bertulani, X.X.Xu New 26P(p, γ)27S Thermonuclear Reaction Rate and Its Astrophysical Implications in the rp-process NUCLEAR REACTIONS 26P(p, γ), E<400 keV; analyzed available data; deduced direct, resonant, and total reaction rates, discrepancies with JINA REACLIB library.
doi: 10r3847/1538-4357/accf9c
2023KE10 Astrophys.J.Suppl.Ser. 268, 8 (2023) J.D.Keegans, M.Pignatari, R.J.Stancliffe, C.Travaglio, S.Jones, B.K.Gibson, D.M.Townsley, B.J.Miles, Ken J.Shen, G.Few Type Ia Supernova Nucleosynthesis: Metallicity-dependent Yields
doi: 10.3847/1538-4365/ace102
2023LA06 J.Phys.(London) G50, 033002 (2023) A.M.Laird, M.Lugaro, A.Kankainen, P.Adsley, D.W.Bardayan, H.E.Brinkman, B.Cote, C.M.Deibel, R.Diehl, F.Hammache, J.W.den Hartogh, J.Jose, D.Kurtulgil, C.Lederer-Woods, G.Lotay, G.Meynet, S.Palmerini, M.Pignatari, R.Reifarth, N.de Sereville, A.Sieverding, R.J.Stancliffe, T.C.L.Trueman, T.Lawson, J.S.Vink, C.Massimi, A.Mengoni Progress on nuclear reaction rates affecting the stellar production of 26Al NUCLEAR REACTIONS 25Mg, 25,26Al(p, γ), 26Al(n, p), (n, α), 25Mg(α, n), 23Na(α, p), 24,25Mg(n, γ), E<300 KeV; analyzed available data; deduced σ, reaction rates, resonance parameters.
doi: 10.1088/1361-6471/ac9cf8
2023LU02 Eur.Phys.J. A 59, 53 (2023) M.Lugaro, M.Ek, M.Peto, M.Pignatari, G.V.Makhatadze, I.J.Onyett, M.Schonbachler Representation of s-process abundances for comparison to data from bulk meteorites
doi: 10.1140/epja/s10050-023-00968-y
2023PI08 Eur.Phys.J. A 59, 302 (2023) M.Pignatari, R.Gallino, R.Reifarth The s process in massive stars, a benchmark for neutron capture reaction rates
doi: 10.1140/epja/s10050-023-01206-1
2022LU09 Universe 8, 343 (2022) M.Lugaro, A.Yague Lopez, B.Soos, B.Cote, M.Peto, N.Vassh, B.Wehmeyer, M.Pignatari Origin of Plutonium-244 in the Early Solar System ATOMIC MASSES 127,129In, 235,238U, 244Pu, 247Cm; calculated ratios of abundances of 129I/127I, 129I/247Cm, 244Pu/238U, and 247Cm/235U produced as short-lived radionucldies (SLRs) in r-process, and present in the early Solar System (ESS) using nuclear network code WINNET with 63 different models, and the nucleosynthesis network PRISM with 14 different models, with detailed results listed in the Supplementary Materials of the paper. 244Pu; discussed different possibilities, solutions, and derived time intervals for the presence of this isotope in early Solar System.
doi: 10.3390/universe8070343
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
2021HU13 Astrophys.J. 912, 59 (2021) N.J.Hubbard, C.Aa.Diget, S.P.Fox, H.O.U.Fynbo, A.M.Howard, O.S.Kirsebom, A.M.Laird, M.Munch, A.Parikh, M.Pignatari, J.R.Tomlinson New Experimental 23Na(α, p)26Mg Reaction Rate for Massive Star and Type Ia Supernova Models NUCLEAR REACTIONS 23Na(α, p), E(cm)=1-3.25 MeV; analyzed available data; deduced astrophysical reaction rates, angle integrated σ.
doi: 10.3847/1538-4357/abee91
2021OT02 Phys.Rev. C 104, 055806 (2021) S.Ota, G.Christian, W.N.Catford, G.Lotay, M.Pignatari, U.Battino, E.A.Bennett, S.Dede, D.T.Doherty, S.Hallam, F.Herwig, J.Hooker, C.Hunt, H.Jayatissa, A.Matta, M.Moukaddam, E.Rao, G.V.Rogachev, A.Saastamoinen, D.Scriven, J.A.Tostevin, S.Upadhyayula, R.Wilkinson (6Li, d) and (6Li, t) reactions on 22Ne and implications for s-process nucleosynthesis NUCLEAR REACTIONS 6Li(22Ne, d)26Mg, 6Li(22Na, t)25Mg, E=154 MeV; 2H(22Ne, p)23Ne, E not given; measured reaction products, E(d), I(d), E(p), I(p), Eγ, Iγ, 26Mg and 25Mg recoils, (26Mg)γ-coin, (25Mg)γ-coin, (particle)(particle)-coin, σ(θ) using TIARA Si detector array of two sets of Si detectors, 'Hyball' and 'Barrel', MDM high-resolution and broad range magnetic spectrometer, and array of four HPGe detectors at the K150 cyclotron of Texas A and M University. 23Ne, 25Mg, 26Mg; deduced levels, J, π, resonances, resonances in the Gamow window of 22Ne(α, n)25Mg reaction, spectroscopic factors, α-spectroscopic factors for 26Mg, resonance strengths, impact of 22Ne+α resonances on s-process nucleosynthesis; comparison of σ(θ) data with DWBA calculations using FRESCO code. Comparison with previous experimental results. 22Ne(α, n), (α, γ); calculated s-process overproduction factors in stars 3 and 5 times the mass of the sun for A=60-210 isotopes.
doi: 10.1103/PhysRevC.104.055806
2021YA29 Astrophys.J. 919, 84 (2021) S.Q.Yan, X.Y.Li, K.Nishio, M.Lugaro, Z.H.Li, H.Makii, M.Pignatari, Y.B.Wang, R.Orlandi, K.Hirose The 59Fe(n, γ)60Fe Cross Section from the Surrogate Ratio Method and Its Effect on the 60Fe Nucleosynthesis NUCLEAR REACTIONS 56,58Fe(18O, 16O), E=103 MeV; measured reaction products, Eγ, Iγ; deduced σ, Maxwellian-averaged σ. Comparison with TALYS calculations.
doi: 10.3847/1538-4357/ac12ce
2020ME09 Phys.Rev. C 102, 035803 (2020) A.Meyer, N.de Sereville, A.M.Laird, F.Hammache, R.Longland, T.Lawson, M.Pignatari, L.Audouin, D.Beaumel, S.Fortier, J.Kiener, A.Lefebvre-Schuhl, M.G.Pellegriti, M.Stanoiu, V.Tatischeff Evaluation of the 13N(α, p)16O thermonuclear reaction rate and its impact on the isotopic composition of supernova grains NUCLEAR REACTIONS 13C(7Li, t)17O*, E=34 MeV; measured E(t), I(t), σ(θ) using Enge Split-Pole magnetic spectrometer at the Tandem-ALTO facility in Orsay. 17O; deduced levels, resonances, J, π, L-transfers from analysis of angular distributions with finite-range distorted wave Born approximation (DWBA) calculations, Γα, α-spectroscopic factors, and compared with previous experimental data, and evaluated data in the ENSDF database. 17O, 17F; comparison of levels resonances, spin-parities, and resonance parameters in mirror nuclei. 13N(α, p)16O, E(cm)=0.05-3.0 MeV; deduced astrophysical S-factor by R-matrix calculations using AZURE2 code, Monte-Carlo reaction rates from 0.01-10 GK, isotopic abundances in the He-shell ejecta of a supernova model, production factors of stable isotopes, in the mass region between 12C and 50V.
doi: 10.1103/PhysRevC.102.035803
2020RI06 Phys.Rev. C 102, 025801 (2020) W.A.Richter, B.A.Brown, R.Longland, C.Wrede, P.Denissenkov, C.Fry, F.Herwig, D.Kurtulgil, M.Pignatari, R.Reifarth Shell-model studies of the astrophysical rp-process reactions 34S(p, γ)35Cl and 34g, mCl(p, γ)35Ar NUCLEAR REACTIONS 34S(3He, d)35Cl, E=20 MeV; calculated spectroscopic factors for levels in 35Cl up to 7.4 MeV using shell model, and compared with experimental values. 34S(p, γ)35Cl, 34,34mCl(p, γ)35Ar, E not given; calculated levels, resonances, J, π, spectroscopic factors, Γp, Γγ, resonance strengths, thermonuclear reaction rates; discussed impact on predicted 34S/32S isotopic ratio for presolar nova grains. Comparison with experimental data. Shell-model approach, with uncertainties estimated using a Monte Carlo method.
doi: 10.1103/PhysRevC.102.025801
2019TA20 Phys.Lett. B 798, 134894 (2019) M.P.Taggart, C.Akers, A.M.Laird, U.Hager, C.Ruiz, D.A.Hutcheon, M.A.Bentley, J.R.Brown, L.Buchmann, A.A.Chen, J.Chen, K.A.Chipps, A.Choplin, J.M.D'Auria, B.Davids, C.Davis, C.Aa.Diget, L.Erikson, J.Fallis, S.P.Fox, U.Frischknecht, B.R.Fulton, N.Galinski, U.Greife, R.Hirschi, D.Howell, L.Martin, D.Mountford, A.St.J.Murphy, D.Ottewell, M.Pignatari, S.Reeve, G.Ruprecht, S.Sjue, L.Veloce, M.Williams A direct measurement of the 17O(α, γ)21Ne reaction in inverse kinematics and its impact on heavy element production NUCLEAR REACTIONS 4He(17O, γ)21Ne, E=160, 202, 290, 360 keV/nucleon; measured reaction products, Eγ, Iγ; deduced resonance strengths, S-factors, astrophysical reaction rates.
doi: 10.1016/j.physletb.2019.134894
2018DE16 J.Phys.(London) G45, 055203 (2018) P.Denissenkov, G.Perdikakis, F.Herwig, H.Schatz, C.Ritter, M.Pignatari, S.Jones, S.Nikas, A.Spyrou The impact of (n, γ) reaction rate uncertainties of unstable isotopes near N = 50 on the i-process nucleosynthesis in He-shell flash white dwarfs NUCLEAR REACTIONS 87,88,89Kr, 85,86Br, 89Rb, 89,92Sr(n, γ), E ∼ 30 keV; calculated mass fractions, astrophysical abundances of Rb, Sr, Y and Zr; deduced an impact of the uncertainties in the (n, γ) reaction rates on Monte Carlo simulation.
doi: 10.1088/1361-6471/aabb6e
2017DE26 Rev.Mod.Phys. 89, 035007 (2017) R.J.deBoer, J.Gorres, M.Wiescher, R.E.Azuma, A.Best, C.R.Brune, C.E.Fields, S.Jones, M.Pignatari, D.Sayre, K.Smith, F.X.Timmes, E.Uberseder The 12C(α, γ)16O reaction and its implications for stellar helium burning NUCLEAR REACTIONS 12C(α, γ)16O, E(cm)<6 MeV; analyzed available data; deduced σ, reaction rates and uncertainties.
doi: 10.1103/RevModPhys.89.035007
2017LI18 Astrophys.J. 842, L1 (2017) N.Liu, L.R.Nittler, M.Pignatari, C.M.O'D.Alexander, J.Wang Stellar Origin of 15N-rich Presolar SiC Grains of Type AB: Supernovae with Explosive Hydrogen Burning
doi: 10.3847/2041-8213/aa74e5
2017MA15 Phys.Lett. B 768, 1 (2017) C.Massimi, S.Altstadt, J.Andrzejewski, L.Audouin, M.Barbagallo, V.Becares, F.Becvar, F.Belloni, E.Berthoumieux, J.Billowes, S.Bisterzo, D.Bosnar, M.Brugger, M.Calviani, F.Calvino, D.Cano-Ott, C.Carrapico, D.M.Castelluccio, F.Cerutti, E.Chiaveri, L.Cosentino, M.Chin, G.Clai, N.Colonna, G.Cortes, M.A.Cortes-Giraldo, S.Cristallo, M.Diakaki, C.Domingo-Pardo, I.Duran, R.Dressler, C.Eleftheriadis, A.Ferrari, P.Finocchiaro, K.Fraval, S.Ganesan, A.R.Garcia, G.Giubrone, I.F.Goncalves, E.Gonzalez-Romero, E.Griesmayer, C.Guerrero, F.Gunsing, A.Hernandez-Prieto, D.G.Jenkins, E.Jericha, Y.Kadi, F.Kappeler, D.Karadimos, N.Kivel, P.Koehler, M.Kokkoris, S.Kopecky, M.Krticka, J.Kroll, C.Lampoudis, C.Langer, E.Leal-Cidoncha, C.Lederer, H.Leeb, L.S.Leong, S.Lo Meo, R.Losito, A.Mallick, A.Manousos, J.Marganiec, T.Martinez, P.F.Mastinu, M.Mastromarco, E.Mendoza, A.Mengoni, P.M.Milazzo, F.Mingrone, M.Mirea, W.Mondelaers, A.Musumarra, C.Paradela, A.Pavlik, J.Perkowski, M.Pignatari, L.Piersanti, A.Plompen, J.Praena, J.M.Quesada, T.Rauscher, R.Reifarth, A.Riego, M.S.Robles, C.Rubbia, M.Sabate-Gilarte, R.Sarmento, A.Saxena, P.Schillebeeckx, S.Schmidt, D.Schumann, G.Tagliente, J.L.Tain, D.Tarrio, L.Tassan-Got, A.Tsinganis, S.Valenta, G.Vannini, I.Van Rijs, V.Variale, P.Vaz, A.Ventura, M.J.Vermeulen, V.Vlachoudis, R.Vlastou, A.Wallner, T.Ware, M.Weigand, C.Weiss, R.Wynants, T.Wright, P.Zugec Neutron spectroscopy of 26Mg states: Constraining the stellar neutron source 22Ne(α, n)25Mg NUCLEAR REACTIONS 25Mg(n, γ), (n, X), E<300 KeV; measured reaction products, En, In, Eγ, Iγ; deduced yields, σ, resonance parameters and corresponding excitation energies of the 26Mg compound nucleus, Maxwellian-averaged cross sections, reaction rates for inverse reactions. R-matrix analysis of the experimental data.
doi: 10.1016/j.physletb.2017.02.025
2017PI16 Geochim.Cosmochim.Act. 221, 37 (2017) M.Pignatari, P.Hoppe, R.Trappitsch, C.Fryer, F.X.Timmes, F.Herwig, R.Hirschi The neutron capture process in the He shell in core-collapse supernovae: Presolar silicon carbide grains as a diagnostic tool for nuclear astrophysics ATOMIC MASSES 90,96Zr, 90Sr, 95,96,97,100Mo; analyzed isotopic abundances in carbon-rich presolar grains; deduced parameters of supernova models.
doi: 10.1016/j.gca.2017.06.005
2017UB01 Phys.Rev. C 95, 025803 (2017) E.Uberseder, M.Heil, F.Kappeler, C.Lederer, A.Mengoni, S.Bisterzo, M.Pignatari, M.Wiescher Stellar (n, γ) cross sections of 23Na NUCLEAR REACTIONS 23Na(n, γ)24Na, E=quasistellar thermal neutrons with kT=5.1-25 keV; measured neutron spectra, Eγ, Iγ, Maxwellian averaged σ(E) (MACS) by activation method using NaCl target at Karlsruhe Van de Graaff accelerator; σ(E) analyzed by R-matrix method using SAMMY code. Comparison with ENDF/B-VII.1 evaluation. Calculated relative s-abundance distribution at the end of C-shell burning with the MACS of 23Na from the KADONIS database compilation, ratio of s-process yields.
doi: 10.1103/PhysRevC.95.025803
2017WA27 Phys.Rev. C 96, 025808 (2017) A.Wallner, K.Buczak, T.Belgya, M.Bichler, L.Coquard, I.Dillmann, R.Golser, F.Kappeler, A.Karakas, W.Kutschera, C.Lederer, A.Mengoni, M.Pignatari, A.Priller, R.Reifarth, P.Steier, L.Szentmiklosi Precise measurement of the thermal and stellar 54Fe (n, γ) cross sections via accelerator mass spectrometry NUCLEAR REACTIONS 54Fe(n, γ), E=cold to 100 keV; measured 55Fe concentration using accelerator mass spectrometry (AMS) technique at the Vienna Environmental Research Accelerator (VERA) laboratory; deduced σ(E), Maxwellian-averaged cross sections (MACS) between 5-100 keV, 55Fe/56Fe ratios. Comparison with previous measurements, and with evaluated data libraries ENDF/B-VII.1, JENDL-4.0, and JEFF-3.2. Impact of the improved cross sections for neutron capture nucleosynthesis for the AGB stars.
doi: 10.1103/PhysRevC.96.025808
2016HE06 Phys.Rev. C 93, 055807 (2016) M.Heil, R.Plag, E.Uberseder, S.Bisterzo, F.Kappeler, A.Mengoni, M.Pignatari Stellar neutron capture cross sections of 41K and 45Sc NUCLEAR REACTIONS 45Sc, 41K(n, γ), kT=25 keV; measured Eγ, Iγ, capture cross section by activation method at Karlsruhe 3.7-MV Van de Graaff accelerator facility; deduced Maxwellian averaged cross sections (MACS) for the s-process nucleosynthesis yields in AGB stars and in massive stars. Comparison with previous experimental values and evaluated libraries JEFF-3.2, JENDL-4.0 and ENDF/B-VII.1. Discussed effect of neutron poisons in s-process scenario.
doi: 10.1103/PhysRevC.93.055807
2016KO01 At.Data Nucl.Data Tables 108, 1 (2016) A.Koloczek, B.Thomas, J.Glorius, R.Plag, M.Pignatari, R.Reifarth, C.Ritter, S.Schmidt, K.Sonnabend Sensitivity study for s process nucleosynthesis in AGB stars COMPILATION 13C, 80,82,83,84,86Kr; analyzed reaction rates in the main component of the s process; deduced 22 rates, which have the highest impact on the s-process abundances in AGB stars.
doi: 10.1016/j.adt.2015.12.001
2016MO23 Astrophys.J. 827, 29 (2016) P.Mohr, C.Heinz, M.Pignatari, I.Dillmann, A.Mengoni, F.Kappeler Re-evaluation of the 16O(N, γ)17O Cross Section at Astrophysical Energies and Its Role as a Neutron Poison in the s-process NUCLEAR REACTIONS 16O(n, γ), E<700 KeV; analyzed available experimental data from KADoNiS and REACLIB, ENDF/B-VII.1, JEFF-3.2, JENDL-4.0 evaluated libraries; deduced Maxwellian-averaged σ, reaction rates.
doi: 10.3847/0004-637X/827/1/29
2016PI06 Int.J.Mod.Phys. E25, 1630003 (2016) M.Pignatari, K.Gobel, R.Reifarth, C.Travaglio The production of proton-rich isotopes beyond iron: The γ-process in stars
doi: 10.1142/S0218301316300034
2016TA09 Phys.Rev. C 93, 055803 (2016) R.Talwar, T.Adachi, G.P.A.Berg, L.Bin, S.Bisterzo, M.Couder, R.J.deBoer, X.Fang, H.Fujita, Y.Fujita, J.Gorres, K.Hatanaka, T.Itoh, T.Kadoya, A.Long, K.Miki, D.Patel, M.Pignatari, Y.Shimbara, A.Tamii, M.Wiescher, T.Yamamoto, M.Yosoi Probing astrophysically important states in the 26Mg nucleus to study neutron sources for the s process NUCLEAR REACTIONS 26Mg(α, α'), E=206 MeV; 22Ne(6Li, d)26Mg, E=82.3 MeV; measured Eα, Iα, E(d), I(d), σ(θ) using Grand Raiden (GR) spectrometer at RCNP-Osaka. 26Mg; deduced α-unbound resonance energies, levels, J, π, α-spectroscopic factors, resonance strengths. Angular distributions for inelastic scattering analyzed by coupled channel code PTOLEMY and for transfer reactions by FRESCO code. 22Ne(α, γ)26Mg, 22Ne(α, n)25Mg, T9=0.01-10; deduced astrophysical reaction rates from resonance parameters. Comparison with previous results. Relevance to slow neutron capture process (s process) in massive stars.
doi: 10.1103/PhysRevC.93.055803
2015BU08 Phys.Rev.Lett. 114, 251102 (2015) B.Bucher, X.D.Tang, X.Fang, A.Heger, S.Almaraz-Calderon, A.Alongi, A.D.Ayangeakaa, M.Beard, A.Best, J.Browne, C.Cahillane, M.Couder, R.J.deBoer, A.Kontos, L.Lamm, Y.J.Li, A.Long, W.Lu, S.Lyons, M.Notani, D.Patel, N.Paul, M.Pignatari, A.Roberts, D.Robertson, K.Smith, E.Stech, R.Talwar, W.P.Tan, M.Wiescher, S.E.Woosley First Direct Measurement of 12C(12C, n)23Mg at Stellar Energies NUCLEAR REACTIONS 12C(12C, n), E=7.5, 9.5 MeV; measured reaction products, Eγ, Iγ, En, In; deduced yields, S-factors, astrophysical reaction rate. Comparison with available data.
doi: 10.1103/PhysRevLett.114.251102
2014HE25 Phys.Rev. C 90, 045804 (2014); Erratum Phys.Rev. C 92, 019902 (2015) M.Heil, R.Plag, E.Uberseder, R.Gallino, S.Bisterzo, A.Juseviciute, F.Kappeler, C.Lederer, A.Mengoni, M.Pignatari Stellar neutron capture cross sections of 20, 21, 22Ne NUCLEAR REACTIONS 20,21,22Ne(n, γ), E=5-800 keV; measured transmission data, σ(E) via prompt γ-ray cascades, and using the TOF technique at the Karlsruhe Van de Graaff accelerator. 21,22,23Ne; deduced energies of neutron resonances, resonance parameters, widths, capture kernels, stellar cross sections (MACS) at kT=30 keV, relative s-abundance distributions. R-matrix analysis using SAMMY code. Comparison with previous experimental results and data in KADONIS database. Discussed 22Ne and 20Ne as significant neutron poisons for the s process in stars.
doi: 10.1103/PhysRevC.90.045804
2014PR07 Nucl.Data Sheets 120, 205 (2014) J.Praena, P.F.Mastinu, M.Pignatari, J.M.Quesada, R.Capote, Y.Morilla Measurement of the MACS of 159Tb(n, γ) at kT=30 keV by Activation NUCLEAR REACTIONS 159Tb(n, γ), E=30 keV; measured reaction products, Eγ, Iγ.; deduced Maxwellian-averaged σ. Comparison with available data, ENDF/B-VII.1 and KADoNiS libraries.
doi: 10.1016/j.nds.2014.07.047
2013BE11 Phys.Rev. C 87, 045805 (2013) A.Best, M.Beard, J.Gorres, M.Couder, R.deBoer, S.Falahat, R.T.Guray, A.Kontos, K.-L.Kratz, P.J.LeBlanc, Q.Li, S.O'Brien, N.Ozkan, M.Pignatari, K.Sonnabend, R.Talwar, W.Tan, E.Uberseder, M.Wiescher Measurement of the reaction 17O(α, n)20Ne and its impact on the s process in massive stars NUCLEAR REACTIONS 17O(α, n), E=800-2300 keV; measured Eγ, Iγ, E(n), I(n), yields as function of incident Eα for (α, n0) and (α, n1) channels; deduced R-matrix parameters, S factors, reaction rates. 21Ne; deduced levels, resonances, J, π, width, resonance strengths. R-matrix analyses. 17O(α, n), (α, γ), E at 0.1 to 10 GK; comparison of experimental and theoretical (NACRE, CF88/1000) reaction rates. Hauser-Feshbach theory. Astrophysical implications for the s-process, and elemental abundance.
doi: 10.1103/PhysRevC.87.045805
2013PR06 Nucl.Instrum.Methods Phys.Res. A727, 1 (2013) J.Praena, P.F.Mastinu, M.Pignatari, J.M.Quesada, J.Garcia-Lopez, M.Lozano, N.Dzysiuk, R.Capote, G.Martin-Hernandez Measurement of the MACS of 181Ta(n, γ) at kT=30 KeV as a test of a method for Maxwellian neutron spectra generation NUCLEAR REACTIONS 181Ta, 197Au(n, γ), E<120 keV; measured reaction products, Eγ, Iγ; deduced Maxwellian-averaged σ. Comparison with experimental results, ENDF libraries.
doi: 10.1016/j.nima.2013.05.151
2012DR08 J.Phys.(London) G39, 105201 (2012) R.Dressler, M.Ayranov, D.Bemmerer, M.Bunka, Y.Dai, C.Lederer, J.Fallis, A.StJ.Murphy, M.Pignatari, D.Schumann, T.Stora, T.Stowasser, F.-K.Thielemann, P.J.Woods 44Ti, 26Al and 53Mn samples for nuclear astrophysics: the needs, the possibilities and the sources
doi: 10.1088/0954-3899/39/10/105201
2012MA29 Appl.Radiat.Isot. 70, 1583 (2012) G.Martin-Hernandez, P.F.Mastinu, J.Praena, N.Dzysiuk, R.Capote Noy, M.Pignatari Temperature-tuned Maxwell-Boltzmann neutron spectra for kT ranging from 30 up to 50 keV for nuclear astrophysics studies NUCLEAR REACTIONS 82Se(n, γ), E<100 keV; calculated Maxwellian-averaged σ and their uncertainties, stellar neutron spectra, σ(E). Comparison with available data.
doi: 10.1016/j.apradiso.2012.05.004
2010BE40 J.Phys.:Conf.Ser. 202, 012023 (2010) M.E.Bennett, R.Hirschi, M.Pignatari, S.Diehl, C.Fryer, F.Herwig, A.Hungerford, G.Magkotsios, G.Rockefeller, F.Timmes, M.Wiescher, P.Young The effect of 12C + 12C rate uncertainties on s-process yields NUCLEAR REACTIONS 12C(12C, p), (12C, α), E≈50-100 keV;23Na(p, α), E≈50-100 keV; calculated 12C burning rates. A≈12-96 calculated isotope yields based on these burning rates in massive stars for s-process.
doi: 10.1088/1742-6596/202/1/012023
2010PI15 Astrophys.J. 710, 1557 (2010) M.Pignatari, R.Gallino, M.Heil, M.Wiescher, F.Kappeler, F.Herwig, S.Bisterzo The Weak s-Process in Massive Stars and its Dependence on the Neutron Capture Cross Sections NUCLEAR REACTIONS 74Ge, 75As, 78Se, 36S, 80Kr(n, γ), E ∼ 30 keV; analyzed available data; deduced Maxwellian averaged σ.
doi: 10.1088/0004-637x/710/2/1557
2009MA35 Phys.Rev. C 79, 065802 (2009) J.Marganiec, I.Dillmann, C.Domingo Pardo, F.Kappeler, R.Reifarth, R.Gallino, M.Pignatari, P.Grabmayr Neutron capture cross sections of 74Ge, 76Ge, and 75As at 25 keV NUCLEAR REACTIONS 74,76Ge, 75As(n, γ), E<106 keV; measured Eγ, Iγ, σ; deduced Maxwellian averaged σ for thermal energies from 5 to 100 keV. Neutrons from 7Li(p, n), E=1912 keV reaction. 197Au(n, γ), E<106 keV; measured σ and used as a standard. Estimated background contributions for γ-ray studies of double β decay of 76Ge.
doi: 10.1103/PhysRevC.79.065802
2009UB01 Phys.Rev.Lett. 102, 151101 (2009) E.Uberseder, R.Reifarth, D.Schumann, I.Dillmann, C.Domingo Pardo, J.Gorres, M.Heil, F.Kappeler, J.Marganiec, J.Neuhausen, M.Pignatari, F.Voss, S.Walter, M.Wiescher Measurement of the 60Fe(n, γ)61Fe Cross Section at Stellar Temperatures NUCLEAR REACTIONS 60Fe(n, γ), E=25-100 keV; measured reaction products, Eγ, Iγ; deduced Maxwellian-averaged σ and its uncertainties. Comparison with stellar models and NACRE data.
doi: 10.1103/PhysRevLett.102.151101
2008HE01 Phys.Rev. C 77, 015808 (2008) M.Heil, F.Kappeler, E.Uberseder, R.Gallino, M.Pignatari Neutron capture cross sections for the weak s process in massive stars NUCLEAR REACTIONS 58Fe, 59Co, 64Ni, 63,65Cu(n, γ), E=25 keV; measured neutron capture cross sections, Eγ; 59Fe, 60Co, 65Ni, 64,66Cu, 198Au; deduced nucleosynthesis yields in stars.
doi: 10.1103/PhysRevC.77.015808
2008HE10 Phys.Rev. C 78, 025802 (2008) M.Heil, F.Kappeler, E.Uberseder, R.Gallino, S.Bisterzo, M.Pignatari Stellar (n, γ) cross sections for Br and Rb: Matching the weak and main s-process components NUCLEAR REACTIONS 79,81Br, 85,87Rb(n, γ), E=0-120 keV; measured Eγ, Iγ, σ. 78,80,82Se, 79,81Br, 80,82,83,84,86Kr; 85,87Rb, 86,87,88Sr, 89Y, 90Zr; deduced total s-process abundances.
doi: 10.1103/PhysRevC.78.025802
2008ST11 Phys.Rev. C 77, 055801 (2008) E.Strandberg, M.Beard, M.Couder, A.Couture, S.Falahat, J.Gorres, P.J.LeBlanc, H.Y.Lee, S.O'Brien, A.Palumbo, E.Stech, W.P.Tan, C.Ugalde, M.Wiescher, H.Costantini, K.Scheller, M.Pignatari, R.Azuma, L.Buchmann 24Mg(α, γ)28Si resonance parameters at low alpha-particle energies NUCLEAR REACTIONS 24Mg(α, γ), E=1.0-1.5 MeV; measured Eγ, Iγ, γγ-coin, branching ratios, resonance strengths. 28Si; deduced levels, J, π, reaction rates. 13C, 17O, 21,22Ne, 25Mg(α, n); 16O, 20Ne(α, γ); 23Na, 24Mg, 27Al(p, γ); 23Na, 24Mg, 27Al, 28Si(n, γ); 25Al(γ, p); 27Al(p, α); analyzed reaction rates.
doi: 10.1103/PhysRevC.77.055801
2007HE14 Prog.Part.Nucl.Phys. 59, 174 (2007) M.Heil, F.Kappeler, E.Uberseder, R.Gallino, M.Pignatari The s process in massive stars
doi: 10.1016/j.ppnp.2006.12.013
2006WI11 Phys.Rev. C 73, 045807 (2006) K.Wisshak, F.Voss, F.Kappeler, L.Kazakov, F.Becvar, M.Krticka, R.Gallino, M.Pignatari Fast neutron capture on the Hf isotopes: Cross sections, isomer production, and stellar aspects NUCLEAR REACTIONS 176,177,178,179,180Hf(n, γ), E=3-225 keV; measured Eγ, Iγ, capture σ; deduced Maxwellian-averaged σ. Astrophysical implications discussed.
doi: 10.1103/PhysRevC.73.045807
2006WI20 Astrophys.J. 647, 685 (2006) N.Winckler, S.Dababneh, M.Heil, F.Kappeler, R.Gallino, M.Pignatari Lanthanum: An s- and r-Process Indicator NUCLEAR REACTIONS 139La(n, γ), E=5.1 keV; measured reaction products, Eγ, Iγ; deduced Maxwellian-averaged σ and its uncertainties.
doi: 10.1086/505026
2005BI19 Nucl.Phys. A758, 284c (2005) S.Bisterzo, L.Pompeia, R.Gallino, M.Pignatari, K.Cunha, A.Heger, V.Smith Cu and Zn in different stellar populations: Inferring their astrophysical origin
doi: 10.1016/j.nuclphysa.2005.05.049
2005PI19 Nucl.Phys. A758, 541c (2005) M.Pignatari, R.Gallino, F.Kappeler, M.Wiescher Effects of uncertainties of the 22Ne(α, n)25Mg and 13C(α, n)16O reaction rates in the s-process yields NUCLEAR REACTIONS 13C, 22Ne(α, n), E=low; analyzed astrophysical reaction rates.
doi: 10.1016/j.nuclphysa.2005.05.098
2003OB03 Phys.Rev. C 68, 035801 (2003) S.O'Brien, S.Dababneh, M.Heil, F.Kappeler, R.Plag, R.Reifarth, R.Gallino, M.Pignatari Neutron capture cross section of 139La NUCLEAR REACTIONS 139La(n, γ), E=spectrum; measured capture σ; deduced Maxwellian-averaged capture σ. Activation technique. Astrophysical implications discussed.
doi: 10.1103/PhysRevC.68.035801
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