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Search: Author = M.Limongi

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2021CH38 Astrophys.J. 916, 79 (2021)

A.Chieffi, L.Roberti, M.Limongi, M.La Cognata, L.Lamia, S.Palmerini, R.G.Pizzone, R.Sparta, A.Tumino

Impact of the New Measurement of the ¹²C + ¹²C Fusion Cross Section on the Final Compactness of Massive Stars

NUCLEAR REACTIONS ¹²C(¹²C, X)²⁴Mg, E<1 MeV; analyzed available data; deduced impact on the dependence of the compactness on the initial mass with respect to previous findings by adopting the classical cross section.

doi: 10.3847/1538-4357/ac06ca
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2021TE06 Phys.Rev. C 104, 015806 (2021)

M.Tessler, J.Zappala, S.Cristallo, L.Roberti, M.Paul, S.Halfon, T.Heftrich, W.Jiang, D.Kijel, A.Kreisel, M.Limongi, Z.-T.Lu, P.Muller, R.Purtschert, R.Reifarth, A.Shor, D.Veltum, D.Vescovi, M.Weigand, L.Weissman

Stellar s-process neutron capture cross sections on ^{78, 80, 84, 86}Kr determined via activation, atom trap trace analysis, and decay counting

NUCLEAR REACTIONS ^78,80,84,86Kr(n, γ)⁷⁹Kr/^79mKr/⁸⁰Kr/⁸¹Kr/^81mKr/⁸⁴Kr/⁸⁵Kr/^85mKr/⁸⁷Kr, kT=42.5 keV, quasi-Maxwellian; ^80,86Kr(γ, n)⁷⁹Kr/^85mKr, E=14.6, 17.6 MeV; measured Eγ, Iγ, average σ(E), ⁸¹Kr/⁸⁰Kr and ⁸⁵Kr/⁸⁴Kr isotopic ratios in (n, γ) reactions by activation method, Atom Trap Trace Analysis (ATTA) and decay counting at SARAF-LiLiT facility, Argonne National Laboratory and low-level counting (LLC) facility of the University of Bern; deduced Maxwellian-averaged cross sections (MACS) at kt=3-300 keV, and stellar reaction rates for s-process in 0.01-4 GK range for (n, γ) reactions. ¹⁹⁷Au(n, γ)¹⁹⁸Au, kT=42.5 keV; ¹⁹⁷Au(γ, n)¹⁹⁶Au, E=14.6, 17.6 MeV; measured Eγ, Iγ, used as monitor reactions. Comparison with previous experimental cross sections, and with data in JEFF-3.3 library. Discussed astrophysical implications, and impact on s-process calculations of abundances of krypton and neighboring nuclides.

RADIOACTIVITY ⁷⁹Kr(EC); ^85mKr(IT); ^85mKr, ⁸⁷Kr(β^-)[from ^78,84,86Kr(n, γ), kT=42.5 keV]; measured half-lives from γ-decay curves and compared with evaluated data.

doi: 10.1103/PhysRevC.104.015806
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2020PR16 Mon.not.R.Astron.Soc. 491, 1832 (2020)

N.Prantzos, C.Abia, S.Cristallo, M.Limongi, A.Chieffi

Chemical evolution with rotating massive star yields II. A new assessment of the solar s- and r- process components

NUCLEAR REACTIONS ⁷⁰Ge, ⁷⁶Se, ^80,82Kr, ^86,87Sr, ⁹⁶Mo, ¹⁰⁰Ru, ¹⁰⁴Pd, ¹¹⁰Cd, ¹¹⁶Sn, ^122,123,124Te, ^128,130Xe, ^134,136Ba, ¹⁴²Nd, ^148,150Sm, ¹⁵⁴Gd, ¹⁶⁰Dy, ¹⁷⁰Yb, ¹⁷⁶Lu, ¹⁷⁶Hf, ¹⁸⁶Os, ¹⁹²Pt, ¹⁹⁸Hg, ²⁰⁴Pb(n, γ), E ∼ 30 keV; analyzed available s-process only data; calculated s-process abundances.

NUCLEAR REACTIONS ^69,71Ga, ^{70,72,73,74,76}Ge, ⁷⁵As, ^{76,77,78,80,82}Se, ^79,81Br, ^{80,82,83,84,86}Kr, ^85,87Rb, ^86,87,88Sr, ⁸⁹Y, ^{90,91,92,94,96}Zr, ⁹³Nb, ^{95,96,97,98,100}Mo, ^{99,100,101,102,104}Ru, ¹⁰³Rh, ^{104,105,106,108,110}Pd, ^107,109Ag, ^{110,111,112,113,114,116}Cd, ¹¹⁵In, ^{116,117,118,119,120,122,124}Sn, ^121,123Sb, ^{122,123,124,125,126,128,130}Te, ¹²⁷I, ^{128,129,130,131,132,134,136}Xe, ¹³³Cs, ^{134,135,136,137,138}Ba, ¹³⁹La, ^140,142Ce, ¹⁴¹Pr, ^{142,143,144,145,146,148,150}Nd, ^{147,148,149,150,152,154}Sm, ^151,153Eu, ^{154,155,156,157,158,160}Gd, ¹⁵⁹Tb, ^{160,161,162,163,164}Dy, ¹⁶⁵Ho, ^{166,167,169,170}Er, ¹⁶⁹Tm, ^{170,171,172,173,174,176}Yb, ^175,176Lu, ^{176,177,178,179,180}Hf, ¹⁸¹Ta, ^{182,183,184,186}W, ^185,187Re, ^{186,187,188,189,190,192}Os, ^191,193Ir, ^{192,194,195,196,198}Pt, ¹⁹⁷Au, ^{198,199,200,201,202,204}Hg, ^203,205Tl, ^{204,206,207,208}Pb, ²⁰⁹Bi, ²³²Th, ^235,238U(n, γ), E ∼ 30 keV; analyzed available data; calculated s- and r-process abundances.

doi: 10.1093/mnras/stz3154
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2017CH08 Astrophys.J. 836, 79 (2017)

A.Chieffi, M.Limongi

The Synthesis of ⁴⁴Ti and ⁵⁶Ni in Massive Stars

doi: 10.3847/1538-4357/836/1/79
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2010LI53 J.Phys.:Conf.Ser. 202, 012002 (2010)

M.Limongi, A.Chieffi

Presupernova evolution and explosion of massive stars

doi: 10.1088/1742-6596/202/1/012002
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2007GA43 Phys.Rev. C 76, 035802 (2007)

L.R.Gasques, E.F.Brown, A.Chieffi, C.L.Jiang, M.Limongi, C.Rolfs, M.Wiescher, D.G.Yakovlev

Implications of low-energy fusion hindrance on stellar burning and nucleosynthesis

NUCLEAR REACTIONS ¹²C, ¹⁶O(¹⁶O, X), E < 12 MeV; ¹⁶O(¹⁶O, X), E < 15 MeV; analyzed fusion cross sections. Deduced S-factors at astrophysical energies.

doi: 10.1103/PhysRevC.76.035802
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2006LI38 Astrophys.J. 647, 483 (2006)

M.Limongi, A.Chieffi

The nucleosynthesis of ²⁶Al and ⁶⁰Fe in solar metallicity stars extending in mass from 11 to 120 M_solar: The hydrostatic and explosive contributions

doi: 10.1086/505164
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2005LI38 Nucl.Phys. A758, 11c (2005)

M.Limongi, A.Chieffi

²⁶Al and ⁶⁰Fe from massive stars

doi: 10.1016/j.nuclphysa.2005.05.006
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2001CR05 Nucl.Phys. A688, 217c (2001)

S.Cristallo, O.Straniero, R.Gallino, F.Herwig, A.Chieffi, M.Limongi, M.Busso

The Formation of the ¹³C Pocket in Asymptotic Giant Branch Stars and Related Nucleosynthesis

doi: 10.1016/S0375-9474(01)00701-1
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2001DO12 Nucl.Phys. A688, 399c (2001)

I.Dominguez, C.Abia, O.Straniero, A.Chieffi, M.Limongi

The Role of Z = 0 AGB Stars on the Early Chemical Enrichment