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NSR database version of April 11, 2024.

Search: Author = M.Beard

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2023JA13      Astrophys.J. 955, 51 (2023)

R.Jain, E.F.Brown, H.Schatz, A.V.Afanasjev, M.Beard, L.R.Gasques, S.S.Gupta, G.W.Hitt, W.R.Hix, R.Lau, P.Moller, W.J.Ong, M.Wiescher, Y.Xu

Impact of Pycnonuclear Fusion Uncertainties on the Cooling of Accreting Neutron Star Crusts

NUCLEAR REACTIONS 40Mg(40Mg, X)80Cr, 44Mg(40Mg, X)84Cr, 44Mg(44Mg, X)88Cr, 44Mg(38Ne, X)82Ti, 40Mg(38Ne, X)78Ti, 32Ne(32Ne, X)64Ca, 32Ne(30Ne, X)62Ca, 30Ne(30Ne, X)60Ca, 40Mg(24O, X), E not given; calculated abundances, pycnonuclear fusion rates using the reaction network with the thermal evolution code dStar. 56Fe; deduced impact of uncertainties on the depth at which nuclear heat is deposited although the total heating remains constant.

doi: 10.3847/1538-4357/acebc4
Citations: PlumX Metrics


2019LA15      Phys.Rev. C 100, 034614 (2019)

E.Lamere, M.Couder, M.Beard, A.Simon, A.Simonetti, M.Skulski, G.Seymour, P.Huestis, K.Manukyan, Z.Meisel, L.Morales, M.Moran, S.Moylan, C.Seymour, E.Stech

Proton-induced reactions on molybdenum

NUCLEAR REACTIONS 92Mo(p, α)89Nb/89mNb, (p, np)91Mo/91mMo, (p, 2p)91mNb, (p, n)92Tc, (p, γ)93Tc/93mTc, E=10.52, 13.03, 15.07, 16.07, 17.05, 18.07 MeV; 94Mo(p, α)91mNb, (p, np)93mMo, (p, 2n)93Tc/93mTc, (p, n)94Tc/94mTc, E=9.04, 10.06, 11.05, 12.05, 13.04, 14.04, 15.04, 16.06, 17.06, 18.05, 19.06 MeV; 95Mo(p, nα)91mNb, (p, α)92mNb, (p, 2n)94Tc/94mTc, (p, n)95mTc/95mTc, E=10.57, 12.01, 13.02, 4.03, 15.07, 16.03, 17.99, 19.03 MeV; 96Mo(p, nα)92mNb, (p, 2n)95Tc/95mTc, (p, n)96Tc/96mTc, E=8.04, 10.06, 11.07, 11.55, 12.07, 12.55, 13.06, 14.05, 15.05, 16.05, 17.05, 18.05, 19.06 MeV; 97Mo(p, 2n)96Tc/96mTc, (p, n)97mTc, E=9.01, 10.05, 10.98, 11.98, 13.02, 14.02, 15.04 MeV; 98Mo(p, α)95Nb/95mNb, (p, 2n)97mTc, (p, γ)99mTc, E=10.06, 11.06, 12.05, 13.06, 14.05, 15.05, 16.06, 17.06, 18.02, 19.05 MeV; 100Mo(p, nα)96Nb, (p, α)97Nb/97mNb, (p, np)99Mo, (p, 2n)99mTc, (p, γ)101Tc, E=8.01, 9.01, 10.07, 11.01, 12.02, 13.03, 14.03, 15.07, 16.04, 17.03, 18.07, 19.07 MeV; measured Eγ, Iγ, σ(E) by γ-activation method. Comparison with HF calculations using TALYS-1.8 code, and with previous experimental results. Measurement made at the Nuclear Science Laboratory at the University of Notre Dame.

doi: 10.1103/PhysRevC.100.034614
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Data from this article have been entered in the EXFOR database. For more information, access X4 datasetC2413.


2018LA06      Astrophys.J. 859, 62 (2018)

R.Lau, M.Beard, S.S.Gupta, H.Schatz, A.V.Afanasjev, E.F.Brown, A.Deibel, L.R.Gasques, G.W.Hitt, W.R.Hix, L.Keek, P.Moller, P.S.Shternin, A.W.Steiner, M.Wiescher, Y.Xu

Nuclear Reactions in the Crusts of Accreting Neutron Stars

doi: 10.3847/1538-4357/aabfe0
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2018LO11      Phys.Rev. C 97, 054613 (2018)

A.M.Long, T.Adachi, M.Beard, G.P.A.Berg, M.Couder, R.J.deBoer, M.Dozono, J.Gorres, H.Fujita, Y.Fujita, K.Hatanaka, D.Ishikawa, T.Kubo, H.Matsubara, Y.Namiki, S.O'Brien, Y.Ohkuma, H.Okamura, H.J.Ong, D.Patel, Y.Sakemi, Y.Shimbara, S.Suzuki, R.Talwar, A.Tamii, A.Volya, T.Wakasa, R.Watanabe, M.Wiescher, R.Yamada, J.Zenihiro

α-unbound levels in 34Ar from 36Ar(p, t)34Ar reaction measurements and implications for the astrophysical 30S (α, p)33Cl reaction rate

NUCLEAR REACTIONS 36Ar(p, t), E=100 MeV; measured triton spectra, σ(θ) using Grand Raiden spectrograph at RCNP, Osaka. 34Ar; deduced levels, α-unbound states; calculated single proton widths, spin distributions for selected excitation energies, and α-spectroscopic factors using back-shifted Fermi gas (BSFG) model and shell model calculations. Comparison of 34Ar levels in several previous experiments. 30S(α, p)33Cl, T9=0.10-3.0; calculated astrophysical reaction rates at temperatures relevant to x-ray bursts (XRB) using a Monte Carlo approach within a narrow-resonance formalism. Comparison of reaction rates with two standard Hauser-Feshbach model predictions.

doi: 10.1103/PhysRevC.97.054613
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Data from this article have been entered in the XUNDL database. For more information, click here.


2017BE18      Phys.Rev.Lett. 119, 1127501 (2017)

M.Beard, S.M.Austin, R.Cyburt

Enhancement of the Triple Alpha Rate in a Hot Dense Medium

NUCLEAR REACTIONS 4He(α, X)8Be, 8Be(α, X)12C, E<30 MeV; calculated 3α σ, reaction rates; deduced that in hot and dense astrophysical environment the rate of the triple-alpha reaction can increase greatly over the value appropriate for helium burning stars owing to hadronically induced deexcitation of the Hoyle state.

doi: 10.1103/PhysRevLett.119.112701
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2017FA10      Phys.Rev. C 96, 045804 (2017)

X.Fang, W.P.Tan, M.Beard, R.J.deBoer, G.Gilardy, H.Jung, Q.Liu, S.Lyons, D.Robertson, K.Setoodehnia, C.Seymour, E.Stech, B.Vande Kolk, M.Wiescher, R.T.deSouza, S.Hudan, V.Singh, X.D.Tang, E.Uberseder

Experimental measurement of 12C + 16O fusion at stellar energies

NUCLEAR REACTIONS 12C(16O, p), (16O, n), (16O, α), E=8.5-11.7 MeV in steps of 100 or 200 keV; measured Eγ, Iγ, Ep, Ip, pγ-coin, charged particles, partial and total fusion σ(E) at the (ANA) accelerator laboratory (NSL) of University of Notre Dame; deduced S factors, astrophysical reaction rates, uncertainty range of the reaction rate within the temperature range of late stellar burning environments. Results analyzed using Statistical model calculations with SAPPHIRE code. 27Al, 24Mg, 27Si; deduced levels, relative γ strengths of the observed transitions with respect to the strength of the ground state transition of the first excited states.

doi: 10.1103/PhysRevC.96.045804
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Data from this article have been entered in the EXFOR database. For more information, access X4 datasetC2812.


2017LO05      Phys.Rev. C 95, 055803 (2017)

A.M.Long, T.Adachi, M.Beard, G.P.A.Berg, Z.Buthelezi, J.Carter, M.Couder, R.J.deBoer, R.W.Fearick, S.V.Fortsch, J.Gorres, J.P.Mira, S.H.T.Murray, R.Neveling, P.Papka, F.D.Smit, E.Sideras-Haddad, J.A.Swartz, R.Talwar, I.T.Usman, M.Wiescher, J.J.Van Zyl, A.Volya

Indirect study of the stellar 34Ar(α, p)37K reaction rate through 40Ca(p, t)38Ca reaction measurements

NUCLEAR REACTIONS 40Ca(p, t)38Ca, E=100 MeV; measured spectra using the K=600 magnetic spectrograph, triton spectra at K=200 Separated Sector Cyclotron facility of iThemba LABS. 38Ca; deduced levels, α-unbound states, resonances, α-spectroscopic factors. Comparison with previous experimental results. 34Ar(α, p)37K, T9=0.2-3.0; deduced reaction rates as a function of stellar temperature, and compared with theoretical model calculations using NON-SMOKER-v5.0w and TALYS 1.8 codes. Relevance to type I x-ray bursts (XRBs).

doi: 10.1103/PhysRevC.95.055803
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Data from this article have been entered in the XUNDL database. For more information, click here.


2017OZ01      Phys.Rev. C 96, 045805 (2017)

N.Ozkan, R.T.Guray, C.Yalcin, W.P.Tan, A.Aprahamian, M.Beard, R.J.deBoer, S.Almaraz-Calderon, S.Falahat, J.Gorres, Q.Li, A.Sauerwein, K.Sonnabend, M.Wiescher, Zs.Fulop, Gy.Gyurky, E.Somorjai, J.Greene

Proton capture reaction cross section measurements on 162Er as a probe of statistical model calculations

NUCLEAR REACTIONS 162Er(p, γ)163Tm, 162Er(p, n)162Tm, E=4.0-9.0 MeV in steps of 0.5 MeV; measured reaction products, Eγ, Iγ, σ(E) by activation method using the FN tandem accelerator at the University of Notre Dame; deduced S factors. Comparison with Hauser Feshbach (HF) statistical model calculations using NON-SMOKER and TALYS codes.

doi: 10.1103/PhysRevC.96.045805
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Data from this article have been entered in the EXFOR database. For more information, access X4 datasetC2276.


2017SI11      J.Phys.(London) G44, 064006 (2017)

A.Simon, M.Beard, B.S.Meyer, B.Roach

Impact of the α optical model potential on the γ-process nucleosynthesis

NUCLEAR REACTIONS 156,158,160Dy, 152,154Er, 168Yb(α, γ), E<5 GK; 106Cd, 112Sn, 144Sm, 151Eu, 168Yb, 197Au(α, n), E(cm)<24 MeV; calculated σ, astrophysical reaction rates. NON-SMOKER, TALYS nuclear model codes, comparison with available data.

doi: 10.1088/1361-6471/aa6bb4
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2016MA66      Phys.Rev. C 94, 044304 (2016)

A.Makinaga, R.Massarczyk, M.Beard, R.Schwengner, H.Otsu, T.Al-Abdullah, M.Anders, D.Bemmerer, R.Hannaske, R.John, A.R.Junghans, S.E.Muller, M.Roder, K.Schmidt, A.Wagner

Dipole strength in 80Se for s process and nuclear transmutation of 79Se

NUCLEAR REACTIONS 80Se(γ, γ'), E<11.5 MeV bremsstrahlung beam from γELBE facility at Dresden; measured Eγ, Iγ, energy-integrated σ, γ(θ). 80Se; deduced levels, J, photoabsorption σ(E) and compared to (γ, n) data. 79Se(n, γ), E=1 keV to 9 MeV; calculated σ(E), Maxwellian-averaged cross sections (MACs), reaction rates as a function of temperature from 0.0001 to 10 GK using TALYS code with various input strength functions. 80Se(γ, n), T9=2-5.5; calculated reaction rates using TALYS code with various input strength functions. Comparison with σ data in KADoNiS database.

doi: 10.1103/PhysRevC.94.044304
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Data from this article have been entered in the EXFOR database. For more information, access X4 datasetG0039. Data from this article have been entered in the XUNDL database. For more information, click here.


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
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Data from this article have been entered in the EXFOR database. For more information, access X4 datasetC2168.


2015MU04      J.Phys.(London) G42, 034027 (2015)

M.Mumpower, R.Surman, D.L.Fang, M.Beard, A.Aprahamian

The impact of uncertain nuclear masses near closed shells on the r-process abundance pattern

doi: 10.1088/0954-3899/42/3/034027
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2015MU12      Phys.Rev. C 92, 035807 (2015)

M.R.Mumpower, R.Surman, D.-L.Fang, M.Beard, P.Moller, T.Kawano, A.Aprahamian

Impact of individual nuclear masses on r-process abundances

NUCLEAR STRUCTURE Z=30-75, N=60-130, A=120-210; calculated relevant Q values, neutron capture rates, photodissociation rates, β-decay rates, and β-delayed neutron emission probabilities using the 2012 version of the Finite-Range Droplet Model (FRDM), and by considering variations of individual nuclear masses; deduced influence of uncertainties in individual masses on the r-process abundance distribution.

doi: 10.1103/PhysRevC.92.035807
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2015SI13      Phys.Rev. C 92, 025806 (2015)

A.Simon, M.Beard, A.Spyrou, S.J.Quinn, B.Bucher, M.Couder, P.A.DeYoung, A.C.Dombos, J.Gorres, A.Kontos, A.Long, M.T.Moran, N.Paul, J.Pereira, D.Robertson, K.Smith, E.Stech, R.Talwar, W.P.Tan, M.Wiescher

Systematic study of (α, γ) reactions for stable nickel isotopes

NUCLEAR REACTIONS 58,60,61,62,64Ni(α, γ), E=5-9 MeV; measured Eγ, Iγ, σ(E) using γ-summing detector SuN at Notre Dame tandem (FN) Pelletron accelerator facility; deduced astrophysical reaction rates. Comparison with available experimental data, and with Hauser-Feshbach calculations using TALYS 1.6 code with different combinations of α-optical potentials. nuclear level densities, and E1 γ-ray strength functions. Comparisons with results in NON-SMOKER and BRUSLIB databases.

doi: 10.1103/PhysRevC.92.025806
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Data from this article have been entered in the EXFOR database. For more information, access X4 datasetC2181.


2014BE34      Phys.Rev. C 90, 034619 (2014)

M.Beard, E.Uberseder, R.Crowter, M.Wiescher

Comparison of statistical model calculations for stable isotope neutron capture

NUCLEAR REACTIONS 36S, 37Cl, 38,40Ar, 39,40,41K, 40,42,43,44,46,48Ca, 45Sc, 46,47,48,49,50Ti, 196,198,199,200,201,202,204Hg, 203,205Tl, 204,206,207,208Pb(n, γ), E at kT=30 keV; calculated Maxwellian-averaged neutron capture cross sections (MACS) at 30 keV for 340 stable isotopes with N=20-127, Z=16-82 using statistical Hauser-Feshbach model codes TALYS and NON-SMOKER, and two new HF codes, CIGAR and SAPPHIRE. Comparison with data in KAdoNiS database, and other available experimental data. Note that only 32 isotopes out of a total of 340 isotopes studied are listed here.

doi: 10.1103/PhysRevC.90.034619
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2014MA81      Phys.Rev. C 90, 044301 (2014)

A.Makinaga, R.Massarczyk, R.Schwengner, M.Beard, F.Donau, M.Anders, D.Bemmerer, R.Beyer, R.Hannaske, A.R.Junghans, M.Kempe, T.Kogler, M.Roder, K.Schmidt, A.Wagner

Dipole strength of 181Ta for the evaluation of the 180Ta stellar neutron capture rate

NUCLEAR REACTIONS 181Ta(γ, γ'), E<10 MeV; measured Eγ, Iγ, γγ-coin, photoabsorption σ(E) using the bremsstrahlung facility γ-ELBE at the electron accelerator of Dresden-Rossendorf (HZDR) facility; deduced mean branching ratios and uncertainty range of ground-state transitions from γ-ray cascades, dipole-strength distribution. Comparison with 181Ta(γ, n) experimental data, and QRPA calculations.

NUCLEAR REACTIONS 180,180m,181Ta(n, γ), E<15 MeV; calculated σ(E), Maxwellian-averaged cross sections (MACS). 181Ta(γ, n) at T=2-5.5 GK; 180mTa(n, γ) at T=0.1-1 GK; calculated stellar reaction rates. Calculations using the code TALYS with various models for the input strength function. Comparison with data in KADoNiS database.

doi: 10.1103/PhysRevC.90.044301
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Data from this article have been entered in the EXFOR database. For more information, access X4 datasetM0886.


2014SC01      Nature(London) 505, 62 (2014)

H.Schatz, S.Gupta, P.Moller, M.Beard, E.F.Brown, A.T.Deibel, L.R.Gasques, W.R.Hix, L.Keek, R.Lau, A.W.Steiner, M.Wiescher

Strong neutrino cooling by cycles of electron capture and β- decay in neutron star crusts

NUCLEAR STRUCTURE 105Zr; calculated single-particle energy levels, J, π, hexadecapole deformation parameters.

doi: 10.1038/nature12757
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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
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Data from this article have been entered in the EXFOR database. For more information, access X4 datasetC2007. Data from this article have been entered in the XUNDL database. For more information, click here.


2013BO30      Phys.Rev. C 88, 065802 (2013)

M.Bowers, Y.Kashiv, W.Bauder, M.Beard, P.Collon, W.Lu, K.Ostdiek, D.Robertson

Measurement of the 33S(α, p)36Cl cross section: Implications for production of 36Cl in the early Solar System

NUCLEAR REACTIONS 33S(α, p)36Cl, E=0.70-2.42 MeV/nucleon; measured reaction products, σ(E), 36Cl/Cl ratio using accelerator mass spectrometry (AMS) technique from 36Cl ions extracted from the (α, p) reaction at Notre Dame accelerator facility. Comparison of measured σ with theoretical cross sections used in the early solar system (ESS) irradiation models, and calculated values from NON-SMOKER and TALYS Hauser-Feshbach codes. Relevance to production of τ<100 My in the early Solar System.

doi: 10.1103/PhysRevC.88.065802
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Data from this article have been entered in the EXFOR database. For more information, access X4 datasetC1968.


2013CH39      Bull.Rus.Acad.Sci.Phys. 77, 890 (2013); Izv.Akad.Nauk RAS, Ser.Fiz 77, 978 (2013)

A.I.Chugunov, A.V.Afanasjev, M.Beard, M.Wiescher, D.G.Yakovlev

Simple approximation of cross sections for nuclear reactions involving Z = 3-12, 14 nuclei

NUCLEAR REACTIONS Be, B, C, N, O, F, Ne, Na, Mg, Si(Be, X), B, C, N, O, F, Ne, Na, Mg, Si(B, X), C, N, O, F, Ne, Na, Mg, Si(C, X), N, O, F, Ne, Na, Mg, Si(N, X), O, F, Ne, Na, Mg, Si(O, X), F, Ne, Na, Mg, Si(F, X), Ne, Na, Mg, Si(Ne, X), Na, Mg, Si(Na, X), Mg, Si(Mg, X), Si(Si, X), E not given; San Paulo potential, below the Coulomb barrier energies.

doi: 10.3103/S1062873813070083
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2012AF01      Phys.Rev. C 85, 054615 (2012)

A.V.Afanasjev, M.Beard, A.I.Chugunov, M.Wiescher, D.G.Yakovlev

Large collection of astrophysical S factors and their compact representation

NUCLEAR REACTIONS Be(Be, X), (B, X), (C, X), (N, X), (O, X), (F, X), (Ne, X), (Na, X), (Mg, X), (Si, X), B(B, X), (C, X), (N, X), (O, X), (F, X), (Ne, X), (Na, X), (Mg, X), (Si, X), C(C, X), (N, X), (F, X), (O, X), (Ne, X), (Na, X), (Mg, X), (Si, X), N(N, X), (O, X), (F, X), (Ne, X), (Na, X), (Mg, X), (Si, X), O(O, X), (F, X), (Ne, X), (Na, X), (Mg, X), (Si, X), F(F, X), (Ne, X), (Na, X), (Mg, X), (Si, X), Ne(Ne, X), (Na, X), (Mg, X), (Si, X), Na(Na, X), (Mg, X), (Si, X), Mg(Mg, X), (Si, X), Si(Si, X), E<39.8 MeV; calculated astrophysical S factors as function of incident energy for A=8-14 Be, A=9-21 for B, A=10-24 for C, A=11-27 for N, A=12-28 for O, A=17-29 for F, A=18-40 for Ne, A=19-43 for Na, A=20-46 for Mg and A=24-52 for Si for a database of 5000 nonresonant fusion reactions. Sao Paulo method and the barrier penetration model. Comparison with experimental data.

doi: 10.1103/PhysRevC.85.054615
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2012AL23      Phys.Rev. C 86, 065805 (2012); Erratum Phys.Rev. C 88, 059902 (2013)

S.Almaraz-Calderon, W.P.Tan, A.Aprahamian, M.Beard, G.P.A.Berg, B.Bucher, M.Couder, J.Gorres, S.O'Brien, D.Patel, A.Roberts, K.Sault, M.Wiescher, C.R.Brune, T.N.Massey, K.Fujita, K.Hatanaka, D.Ishiwaka, H.Matsubara, H.Okamura, H.J.Ong, Y.Sakemi, Y.Shimizu, T.Suzuki, Y.Tameshige, A.Tamii, J.Zenihiro, T.Kubo, Y.Namiki, Y.Ohkuma, Y.Shimbara, S.Suzuki, R.Watanabe, R.Yamada, T.Adachi, Y.Fujita, H.Fujita, M.Dozono, T.Wakasa

Level structure of 30S and its importance in the 26Si(α, p)29P and 29P(p, γ)30S reaction rates

NUCLEAR REACTIONS 32S(p, t), E=98.7 MeV; measured triton spectra at two angles using Grand Raiden (GR) magnetic spectrometer at RCNP facility. 28Si(3He, n), E=15 MeV; measured neutron (TOF) spectra, charged-particle spectra, (charged-particle)n-coin, angular distributions using LESA array and scintillation detectors at Notre Dame NSL facility. 30S; deduced levels, proton- and α- unbound levels, J, π, proton branching ratios, partial proton widths. DWBA analysis. Comparison with several previous experimental studies. 29P(p, γ)30S, 26Si(α, p)29P, T9=0.01-10 GK; deduced astrophysical reaction rates. Comparison with previous theoretical calculations. Contribution of resonances to total reaction rates.

doi: 10.1103/PhysRevC.86.065805
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Data from this article have been entered in the XUNDL database. For more information, click here.


2012BE22      Phys.Rev. C 85, 065808 (2012)

M.Beard, S.Frauendorf, B.Kampfer, R.Schwengner, M.Wiescher

Photonuclear and radiative-capture reaction rates for nuclear astrophysics and transmutation: 92-100Mo, 88Sr, 90Zr, and 139La

NUCLEAR REACTIONS 92,94,96,98,100Mo, 88Sr, 90Zr, 139La(γ, n), (γ, p), (γ, α), (n, γ), (p, γ), (α, γ), E<16 MeV; calculated γ strength functions, σ(E), stellar reaction rates. Statistical model code TALYS, single Lorentzian (SLO), double Lorentzian (DLO), and generalized Lorentzian (GLO) calculations. Enhancement of radiative capture reaction cross sections by pygmy resonances in 88Sr, 90Zr and 139La. Comparison with experimental data.

doi: 10.1103/PhysRevC.85.065808
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2012SH23      Phys.Rev. C 86, 015808 (2012)

P.S.Shternin, M.Beard, M.Wiescher, D.G.Yakovlev

Neutron degeneracy and plasma physics effects on radiative neutron captures in neutron star crust

NUCLEAR REACTIONS 38Mg(n, γ), E<1.5 MeV; 39Mg(n, γ), E<0.1 MeV; 46Mg(n, γ), E<6 MeV; 62Ca(n, γ), E<10 MeV; calculated astrophysical σ(E), Rn ratios (Fermi-Dirac to Maxwell-Boltzmann cross sections), forward and inverse reaction rates in dense stellar medium with consideration of effects of plasma physics and neutron degeneracy in neutron star crust.

doi: 10.1103/PhysRevC.86.015808
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2011ES06      Phys.Rev.Lett. 107, 172503 (2011)

A.Estrade, M.Matos, H.Schatz, A.M.Amthor, D.Bazin, M.Beard, A.Becerril, E.F.Brown, R.Cyburt, T.Elliot, A.Gade, D.Galaviz, S.George, S.S.Gupta, W.R.Hix, R.Lau, G.Lorusso, P.Moller, J.Pereira, M.Portillo, A.M.Rogers, D.Shapira, E.Smith, A.Stolz, M.Wallace, M.Wiescher

Time-of-Flight Mass Measurements for Nuclear Processes in Neutron Star Crusts

ATOMIC MASSES 53,54,55Sc, 57Ti, 60,61V, 63Cr, 65,66Mn, 67,68Fe, 68,69,70,71Co, 74Ni; measured time of flight; deduced masses. Stellar nucleosynthesis implications.

doi: 10.1103/PhysRevLett.107.172503
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2011MA46      Phys.Rev. C 84, 025801 (2011)

A.Matic, A.M.van den Berg, M.N.Harakeh, H.J.Wortche, M.Beard, G.P.A.Berg, J.Gorres, P.LeBlanc, S.O'Brien, M.Wiescher, K.Fujita, K.Hatanaka, Y.Sakemi, Y.Shimizu, Y.Tameshige, A.Tamii, M.Yosoi, T.Adachi, Y.Fujita, Y.Shimbara, H.Fujita, T.Wakasa, J.P.Greene, R.Crowter, H.Schatz

High-precision 28Si( p, t)26Si reaction to determine 22Mg(α, p)25Al reaction rates

NUCLEAR REACTIONS 28Si(p, t)26Si, E=98.7 MeV; measured E(t), I(t), angular distributions using Grand Raiden spectrometer at RCNP facility. 26Si; deduced levels above the α-emission threshold, J, π, α-resonances, spectroscopic factors. 22Mg(α, p)25Al; deduced stellar reaction rates using the narrow resonance formalism. Comparison with theoretical calculations.

doi: 10.1103/PhysRevC.84.025801
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2010BE12      At.Data Nucl.Data Tables 96, 541 (2010)

M.Beard, A.V.Afanasjev, L.C.Chamon, L.R.Gasques, M.Wiescher, D.G.Yakovlev

Astrophysical S factors for fusion reactions involving C, O, Ne, and Mg isotopes

NUCLEAR REACTIONS C(C, X), (O, X), (Ne, X), (Mg, X), O(O, X), (Ne, X), (Mg, X), Ne(Ne, X), (Mg, X), Mg(Mg, X), E≈18-30 MeV MeV; calculated S-factors; deduced reaction rates calculation procedure.

doi: 10.1016/j.adt.2010.02.005
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2010LE02      Phys.Rev. C 81, 015802 (2010)

H.Y.Lee, J.P.Greene, C.L.Jiang, R.C.Pardo, K.E.Rehm, J.P.Schiffer, A.H.Wuosmaa, N.J.Goodman, J.C.Lighthall, S.T.Marley, K.Otsuki, N.Patel, M.Beard, M.Notani, X.D.Tang

Experimental study of the 11, 12B(n, γ) reactions and their influence on r-process nucleosynthesis of light elements

NUCLEAR REACTIONS 2H(11B, p), E=81 MeV; 2H(12B, p), E=75 MeV; measured proton and 11,12,13B particle spectra, σ(θ). 12,13B; deduced levels, J, π, l-transfers. Comparison with DWBA calculations. 11B, 12B(n, γ); deduced reaction rates of astrophysical relevance, and abundances of 11B and 12B in r process.

doi: 10.1103/PhysRevC.81.015802
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2010LE21      Phys.Rev. C 82, 055804 (2010), Erratum Phys.Rev. C 84, 019902 (2011)

P.J.LeBlanc, G.Imbriani, J.Gorres, M.Junker, R.Azuma, M.Beard, D.Bemmerer, A.Best, C.Broggini, A.Caciolli, P.Corvisiero, H.Costantini, M.Couder, R.deBoer, Z.Elekes, S.Falahat, A.Formicola, Zs.Fulop, G.Gervino, A.Guglielmetti, C.Gustavino, Gy.Gyurky, F.Kappeler, A.Kontos, R.Kuntz, H.Leiste, A.Lemut Q.Li, B.Limata, M.Marta, C.Mazzocchi, R.Menegazzo, S.O'Brien, A.Palumbo, P.Prati, V.Roca, C.Rolfs, C.Rossi Alvarez, E.Somorjai, E.Stech, O.Straniero, F.Strieder, W.Tan, F.Terrasi, H.P.Trautvetter, E.Uberseder, M.Wiescher

Constraining the S factor of 15N(p, γ)16O at astrophysical energies

NUCLEAR REACTIONS 15N(p, γ), E=130-1800 keV; measured Ep, Ip, Eγ, Iγ, σ(E), σ(θ); deduced resonances, branching ratios, astrophysical S factors and reaction rates. Multilevel R-matrix analysis. Implications for the first and second cycles of the CNO cycles.

doi: 10.1103/PhysRevC.82.055804
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2010YA19      Phys.Rev. C 82, 044609 (2010)

D.G.Yakovlev, M.Beard, L.R.Gasques, M.Wiescher

Simple analytic model for astrophysical S factors

NUCLEAR REACTIONS 46Mg(46Mg, X), E=29.9 MeV; 12C(12C, X), E=1-12 MeV; C(C, X), (O, X), E=2-17.9 MeV; C(Ne, X), (Mg, X), O(O, X), E=2-19.9 MeV; O(Ne, X), (Mg, X), Ne(Ne, X), E=2-21.9 MeV; Ne(Mg, X), E=2-24.9 MeV; Mg(Mg, X), E=2-29.9 MeV; calculated astrophysical S factors using a simple model with physically meaningful parameters. Comparison with experimental data.

doi: 10.1103/PhysRevC.82.044609
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2009TA09      Phys.Rev. C 79, 055805 (2009)

W.P.Tan, J.Gorres, M.Beard, M.Couder, A.Couture, S.Falahat, J.L.Fisker, L.Lamm, P.J.LeBlanc, H.Y.Lee, S.O'Brien, A.Palumbo, E.Stech, E.Strandberg, M.Wiescher

Measurement of the decay branching ratios of the α-unbound states in 19Ne and the 15O(α, γ) reaction rate

NUCLEAR REACTIONS 19F(3He, t), E=24 MeV; measured triton spectra, tα-coin, α(θ), α-decay branching ratios. 19Ne; deduced levels, J, π, α-unbound resonances. 15O(α, γ); deduced reaction rates versus temperature.

doi: 10.1103/PhysRevC.79.055805
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2008CO03      Phys.Rev. C 77, 015802 (2008)

A.Couture, M.Beard, M.Couder, J.Gorres, L.Lamm, P.J.LeBlanc, H.Y.Lee, S.O'Brien, A.Palumbo, E.Stech, E.Strandberg, W.Tan, E.Uberseder, C.Ugalde, M.Wiescher, R.Azuma

Measurement of the 19F(p, γ)20Ne reaction and interference terms from Ec.m.=200-760 keV

NUCLEAR REACTIONS 19F(p, γ), E(cm)=200-700 keV; measured Eγ, Iγ, resonance parameters, interference signs. 20Ne, 16O, 19F; deduced levels, J, π.

doi: 10.1103/PhysRevC.77.015802
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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
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2007GA50      Phys.Rev. C 76, 045802 (2007)

L.R.Gasques, A.V.Afanasjev, M.Beard, J.Lubian, T.Neff, M.Wiescher, D.G.Yakovlev

Sao Paulo potential as a tool for calculating S factors of fusion reactions in dense stellar matter

NUCLEAR REACTIONS 16O(16O, X), E(cm)=0-20 MeV; 20O(20O, X), E=0-28 MeV; 20O(26Ne, X), E=0-20 MeV; 20O(32Mg, X), E=0-24 MeV; 26Ne(26Ne, X), E=0-24 MeV; 26Ne(32Mg, X), E=0-28 MeV; 32Mg(32Mg, X), E=0-28 MeV; 22O(22O, X), E=0-20 MeV; 24O(24O, X), E(cm)=0-20 MeV; calculated astrophysical S-factors for fusion reactions. Sao Paulo potential.

doi: 10.1103/PhysRevC.76.045802
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2006YA14      Phys.Rev. C 74, 035803 (2006)

D.G.Yakovlev, L.R.Gasques, A.V.Afanasjev, M.Beard, M.Wiescher

Fusion reactions in multicomponent dense matter

NUCLEAR REACTIONS 12C, 16O(12C, X), (16O, X), E(cm)=0-20 MeV; calculated astrophysical S-factors, fusion rates in dense matter.

doi: 10.1103/PhysRevC.74.035803
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2005GA33      Phys.Rev. C 72, 025806 (2005)

L.R.Gasques, A.V.Afanasjev, E.F.Aguilera, M.Beard, L.C.Chamon, P.Ring, M.Wiescher, D.G.Yakovlev

Nuclear fusion in dense matter: Reaction rate and carbon burning

NUCLEAR REACTIONS 12C(12C, 12C), E(cm)=6-10 MeV; calculated σ(θ). 12C(12C, X), E(cm) ≈ 0-10 MeV; calculated astrophysical S-factor, fusion rate in dense matter.

doi: 10.1103/PhysRevC.72.025806
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2005GA38      Nucl.Phys. A758, 134c (2005)

L.R.Gasques, A.V.Afanasjev, M.Beard, L.C.Chamon, P.Ring, M.Wiescher

Pycnonuclear reaction rates between neutron-rich nuclei

NUCLEAR REACTIONS 22,24O(22O, X), 24O, 34Ne, 42Mg(24O, X), 34Ne, 42Mg(34Ne, X), 42Mg(42Mg, X), E(cm) ≈ 0-18 MeV; calculated S-factors, pycnonuclear reactions rates.

doi: 10.1016/j.nuclphysa.2005.05.027
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2005GA48      J.Phys.(London) G31, S1859 (2005)

L.R.Gasques, M.Beard, L.C.Chamon, M.Wiescher

Pycnonuclear 12C + 12C reaction at zero temperature

NUCLEAR REACTIONS 12C(12C, X), E ≈ 0-10 MeV; calculated astrophysical S-factor, pycnonuclear reaction rate.

doi: 10.1088/0954-3899/31/10/088
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