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1. Improved astrophysical rate for the 18O(p,α)15N reaction by underground measurements

Author

Bruno, Carlo C.G., Aliotta, Marialuisa, Descouvemont, Pierre, Best, Andreas, Davinson, Thomas, Bemmerer, Daniel, Boeltzig, Axel, Broggini, Carlo, Caciolli, Antonio, Cavanna, Francesca, Chillery, Thomas, Ciani, Giacomo G.F., Corvisiero, Pietro, Depalo, Rosanna, Di Leva, Antonino, Elekes, Zoltán, Ferraro, Federico, Formicola, Alba, Fulop, Zsolt, Gervino, Gianpiero, Guglielmetti, Alessandra, Gustavino, Carlo, Gyurky, Gy, Imbriani, Gianluca, Junker, Matthias, Lugaro, Maria, Marigo, Paola, Menegazzo, Roberto, Mossa, Viviana, Pantaleo, Felice F.R., Piatti, D., Prati, Paolo, Stöckel, Klaus, Straniero, Oscar, Strieder, Frank, Szücs, Tamás, Takács, Marcell M.P., Trezzi, Davide, Bruno, Carlo C.G., Aliotta, Marialuisa, Descouvemont, Pierre, Best, Andreas, Davinson, Thomas, Bemmerer, Daniel, Boeltzig, Axel, Broggini, Carlo, Caciolli, Antonio, Cavanna, Francesca, Chillery, Thomas, Ciani, Giacomo G.F., Corvisiero, Pietro, Depalo, Rosanna, Di Leva, Antonino, Elekes, Zoltán, Ferraro, Federico, Formicola, Alba, Fulop, Zsolt, Gervino, Gianpiero, Guglielmetti, Alessandra, Gustavino, Carlo, Gyurky, Gy, Imbriani, Gianluca, Junker, Matthias, Lugaro, Maria, Marigo, Paola, Menegazzo, Roberto, Mossa, Viviana, Pantaleo, Felice F.R., Piatti, D., Prati, Paolo, Stöckel, Klaus, Straniero, Oscar, Strieder, Frank, Szücs, Tamás, Takács, Marcell M.P., and Trezzi, Davide

Abstract

The 18O(p,α)15N reaction affects the synthesis of 15N, 18O and 19F isotopes, whose abundances can be used to probe the nucleosynthesis and mixing processes occurring deep inside asymptotic giant branch (AGB) stars. We performed a low-background direct measurement of the 18O(p,α)15N reaction cross-section at the Laboratory for Underground Nuclear Astrophysics (LUNA) from center of mass energy Ec.m.=340 keV down to Ec.m.=55 keV, the lowest energy measured to date corresponding to a cross-section of less than 1 picobarn/sr. The strength of a key resonance at center of mass energy Er=90 keV was found to be a factor of 10 higher than previously reported. A multi-channel R-matrix analysis of our and other data available in the literature was performed. Over a wide temperature range, T=0.01–1.00 GK, our new astrophysical rate is both more accurate and precise than recent evaluations. Stronger constraints can now be placed on the physical processes controlling nucleosynthesis in AGB stars with interesting consequences on the abundance of 18O in these stars and in stardust grains, specifically on the production sites of oxygen-rich Group II grains., SCOPUS: ar.j, info:eu-repo/semantics/published

Published
2019

2. Underground study of the 17O(p,alpha)18F reaction relevant for explosive hydrogen burning

Author

Universitat Politècnica de Catalunya. Departament de Física i Enginyeria Nuclear, Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica, Di Leva, A, Scott, D.A., Caciolli, A., Formicola, A., Strieder, F., Aliotta, M., Anders, M., Bemmerer, D., Broggini, C., Corvisiero, P., Elekes, Z., Fulop, Zs., Gervino, G., Guglielmetti, G., Gustavino, C., Gyurky, Gy., Imbriani, G., José Pont, Jordi, Junker, M., Universitat Politècnica de Catalunya. Departament de Física i Enginyeria Nuclear, Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica, Di Leva, A, Scott, D.A., Caciolli, A., Formicola, A., Strieder, F., Aliotta, M., Anders, M., Bemmerer, D., Broggini, C., Corvisiero, P., Elekes, Z., Fulop, Zs., Gervino, G., Guglielmetti, G., Gustavino, C., Gyurky, Gy., Imbriani, G., José Pont, Jordi, and Junker, M.

Abstract

The 17O(p,γ )18F reaction affects the production of key isotopes (e.g., 18F and 18O) in the explosive hydrogen burning that powers classical novae. Under these explosive conditions, the reaction rate is dominated by contributions from a narrow resonance at Ec.m.= 183 keV and by the combined contributions of direct capture and low-energy tails of broad resonances. At present, the astrophysical reaction rate is not well constrained because of the lack of data in the energy region appropriate to classical novae., Postprint (published version)

Published
2014

3. Revision of the 15N(p,{\gamma})16O reaction rate and oxygen abundance in H-burning zones

Author

Caciolli, A., Mazzocchi, C., Capogrosso, V., Bemmerer, D., Broggini, C., Corvisiero, P., Costantini, H., Elekes, Z., Formicola, A., Fulop, Zs., Gervino, G., Guglielmetti, A., Gustavino, C., Gyurky, Gy., Imbriani, G., Junker, M., Lemut, A., Marta, M., Menegazzo, R., Palmerini, S., Prati, P., Roca, V., Rolfs, C., Alvarez, C. Rossi, Somorjai, E., Straniero, O., Strieder, F., Terrasi, F., Trautvetter, H. P., Vomiero, A., Caciolli, A., Mazzocchi, C., Capogrosso, V., Bemmerer, D., Broggini, C., Corvisiero, P., Costantini, H., Elekes, Z., Formicola, A., Fulop, Zs., Gervino, G., Guglielmetti, A., Gustavino, C., Gyurky, Gy., Imbriani, G., Junker, M., Lemut, A., Marta, M., Menegazzo, R., Palmerini, S., Prati, P., Roca, V., Rolfs, C., Alvarez, C. Rossi, Somorjai, E., Straniero, O., Strieder, F., Terrasi, F., Trautvetter, H. P., and Vomiero, A.

Abstract

The NO cycle takes place in the deepest layer of a H-burning core or shell, when the temperature exceeds T {\simeq} 30 {\cdot} 106 K. The O depletion observed in some globular cluster giant stars, always associated with a Na enhancement, may be due to either a deep mixing during the RGB (red giant branch) phase of the star or to the pollution of the primordial gas by an early population of massive AGB (asymptotic giant branch) stars, whose chemical composition was modified by the hot bottom burning. In both cases, the NO cycle is responsible for the O depletion. The activation of this cycle depends on the rate of the 15N(p,{\gamma})16O reaction. A precise evaluation of this reaction rate at temperatures as low as experienced in H-burning zones in stellar interiors is mandatory to understand the observed O abundances. We present a new measurement of the 15N(p,{\gamma})16O reaction performed at LUNA covering for the first time the center of mass energy range 70-370 keV, which corresponds to stellar temperatures between 65 {\cdot} 106 K and 780 {\cdot}106 K. This range includes the 15N(p,{\gamma})16O Gamow-peak energy of explosive H-burning taking place in the external layer of a nova and the one of the hot bottom burning (HBB) nucleosynthesis occurring in massive AGB stars. With the present data, we are also able to confirm the result of the previous R-matrix extrapolation. In particular, in the temperature range of astrophysical interest, the new rate is about a factor of 2 smaller than reported in the widely adopted compilation of reaction rates (NACRE or CF88) and the uncertainty is now reduced down to the 10% level., Comment: 6 pages, 5 figures

Published
2011
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4. The 14N(p,gamma)15O reaction studied with a composite germanium detector

Author

Marta, M., Formicola, A., Bemmerer, D., Broggini, C., Caciolli, A., Corvisiero, P., Costantini, H., Elekes, Z., Fulop, Zs., Gervino, G., Guglielmetti, A., Gustavino, C., Gyurky, Gy., Imbriani, G., Junker, M., Lemut, A., Limata, B., Mazzocchi, C., Menegazzo, R., Prati, P., Roca, V., Rolfs, C., Alvarez, C. Rossi, Somorjai, E., Straniero, O., Strieder, F., Terrasi, F., Trautvetter, H. P., Vomiero, A., Marta, M., Formicola, A., Bemmerer, D., Broggini, C., Caciolli, A., Corvisiero, P., Costantini, H., Elekes, Z., Fulop, Zs., Gervino, G., Guglielmetti, A., Gustavino, C., Gyurky, Gy., Imbriani, G., Junker, M., Lemut, A., Limata, B., Mazzocchi, C., Menegazzo, R., Prati, P., Roca, V., Rolfs, C., Alvarez, C. Rossi, Somorjai, E., Straniero, O., Strieder, F., Terrasi, F., Trautvetter, H. P., and Vomiero, A.

Abstract

The rate of the carbon-nitrogen-oxygen (CNO) cycle of hydrogen burning is controlled by the 14N(p,gamma)15O reaction. The reaction proceeds by capture to the ground states and several excited states in O-15. In order to obtain a reliable extrapolation of the excitation curve to astrophysical energy, fits in the R-matrix framework are needed. In an energy range that sensitively tests such fits, new cross section data are reported here for the four major transitions in the 14N(p,gamma)15O reaction. The experiment has been performed at the Laboratory for Underground Nuclear Astrophysics (LUNA) 400 kV accelerator placed deep underground in the Gran Sasso facility in Italy. Using a composite germanium detector, summing corrections have been considerably reduced with respect to previous studies. The cross sections for capture to the ground state and to the 5181, 6172, and 6792 keV excited states in O-15 have been determined at 359, 380, and 399 keV beam energy. In addition, the branching ratios for the decay of the 278 keV resonance have been remeasured., Comment: Submitted to Phys. Rev. C

Published
2011
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5. Revision of the 15N(p,{\gamma})16O reaction rate and oxygen abundance in H-burning zones

Author

Caciolli, A., Mazzocchi, C., Capogrosso, V., Bemmerer, D., Broggini, C., Corvisiero, P., Costantini, H., Elekes, Z., Formicola, A., Fulop, Zs., Gervino, G., Guglielmetti, A., Gustavino, C., Gyurky, Gy., Imbriani, G., Junker, M., Lemut, A., Marta, M., Menegazzo, R., Palmerini, S., Prati, P., Roca, V., Rolfs, C., Alvarez, C. Rossi, Somorjai, E., Straniero, O., Strieder, F., Terrasi, F., Trautvetter, H. P., Vomiero, A., Caciolli, A., Mazzocchi, C., Capogrosso, V., Bemmerer, D., Broggini, C., Corvisiero, P., Costantini, H., Elekes, Z., Formicola, A., Fulop, Zs., Gervino, G., Guglielmetti, A., Gustavino, C., Gyurky, Gy., Imbriani, G., Junker, M., Lemut, A., Marta, M., Menegazzo, R., Palmerini, S., Prati, P., Roca, V., Rolfs, C., Alvarez, C. Rossi, Somorjai, E., Straniero, O., Strieder, F., Terrasi, F., Trautvetter, H. P., and Vomiero, A.

Abstract

The NO cycle takes place in the deepest layer of a H-burning core or shell, when the temperature exceeds T {\simeq} 30 {\cdot} 106 K. The O depletion observed in some globular cluster giant stars, always associated with a Na enhancement, may be due to either a deep mixing during the RGB (red giant branch) phase of the star or to the pollution of the primordial gas by an early population of massive AGB (asymptotic giant branch) stars, whose chemical composition was modified by the hot bottom burning. In both cases, the NO cycle is responsible for the O depletion. The activation of this cycle depends on the rate of the 15N(p,{\gamma})16O reaction. A precise evaluation of this reaction rate at temperatures as low as experienced in H-burning zones in stellar interiors is mandatory to understand the observed O abundances. We present a new measurement of the 15N(p,{\gamma})16O reaction performed at LUNA covering for the first time the center of mass energy range 70-370 keV, which corresponds to stellar temperatures between 65 {\cdot} 106 K and 780 {\cdot}106 K. This range includes the 15N(p,{\gamma})16O Gamow-peak energy of explosive H-burning taking place in the external layer of a nova and the one of the hot bottom burning (HBB) nucleosynthesis occurring in massive AGB stars. With the present data, we are also able to confirm the result of the previous R-matrix extrapolation. In particular, in the temperature range of astrophysical interest, the new rate is about a factor of 2 smaller than reported in the widely adopted compilation of reaction rates (NACRE or CF88) and the uncertainty is now reduced down to the 10% level., Comment: 6 pages, 5 figures

Published
2011
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6. The 14N(p,gamma)15O reaction studied with a composite germanium detector

Author

Marta, M., Formicola, A., Bemmerer, D., Broggini, C., Caciolli, A., Corvisiero, P., Costantini, H., Elekes, Z., Fulop, Zs., Gervino, G., Guglielmetti, A., Gustavino, C., Gyurky, Gy., Imbriani, G., Junker, M., Lemut, A., Limata, B., Mazzocchi, C., Menegazzo, R., Prati, P., Roca, V., Rolfs, C., Alvarez, C. Rossi, Somorjai, E., Straniero, O., Strieder, F., Terrasi, F., Trautvetter, H. P., Vomiero, A., Marta, M., Formicola, A., Bemmerer, D., Broggini, C., Caciolli, A., Corvisiero, P., Costantini, H., Elekes, Z., Fulop, Zs., Gervino, G., Guglielmetti, A., Gustavino, C., Gyurky, Gy., Imbriani, G., Junker, M., Lemut, A., Limata, B., Mazzocchi, C., Menegazzo, R., Prati, P., Roca, V., Rolfs, C., Alvarez, C. Rossi, Somorjai, E., Straniero, O., Strieder, F., Terrasi, F., Trautvetter, H. P., and Vomiero, A.

Abstract

The rate of the carbon-nitrogen-oxygen (CNO) cycle of hydrogen burning is controlled by the 14N(p,gamma)15O reaction. The reaction proceeds by capture to the ground states and several excited states in O-15. In order to obtain a reliable extrapolation of the excitation curve to astrophysical energy, fits in the R-matrix framework are needed. In an energy range that sensitively tests such fits, new cross section data are reported here for the four major transitions in the 14N(p,gamma)15O reaction. The experiment has been performed at the Laboratory for Underground Nuclear Astrophysics (LUNA) 400 kV accelerator placed deep underground in the Gran Sasso facility in Italy. Using a composite germanium detector, summing corrections have been considerably reduced with respect to previous studies. The cross sections for capture to the ground state and to the 5181, 6172, and 6792 keV excited states in O-15 have been determined at 359, 380, and 399 keV beam energy. In addition, the branching ratios for the decay of the 278 keV resonance have been remeasured., Comment: Submitted to Phys. Rev. C

Published
2011
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7. Direct measurement of the 15N(p,gamma)16O total cross section at novae energies

Author

Bemmerer, D, Caciolli, A, Bonetti, R, Broggini, C, Confortola, F, Corvisiero, P, Costantini, H, Elekes, Z, Formicola, A, Fulop, Zs, Gervino, G, Guglielmetti, A, Gustavino, C, Gyurky, Gy, Junker, M, Limata, B, Marta, M, Menegazzo, R, Prati, P, Roca, V, Rolfs, C, Alvarez, C Rossi, Somorjai, E, Straniero, O, Bemmerer, D, Caciolli, A, Bonetti, R, Broggini, C, Confortola, F, Corvisiero, P, Costantini, H, Elekes, Z, Formicola, A, Fulop, Zs, Gervino, G, Guglielmetti, A, Gustavino, C, Gyurky, Gy, Junker, M, Limata, B, Marta, M, Menegazzo, R, Prati, P, Roca, V, Rolfs, C, Alvarez, C Rossi, Somorjai, E, and Straniero, O

Abstract

The 15N(p,gamma)16O reaction controls the passage of nucleosynthetic material from the first to the second carbon-nitrogen-oxygen (CNO) cycle. A direct measurement of the total 15N(p,gamma)16O cross section at energies corresponding to hydrogen burning in novae is presented here. Data have been taken at 90-230 keV center-of-mass energy using a windowless gas target filled with nitrogen of natural isotopic composition and a bismuth germanate summing detector. The cross section is found to be a factor two lower than previously believed., Comment: LUNA collaboration; accepted by J. Phys. G

Published
2009
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8. Precision study of ground state capture in the 14N(p,gamma)15O reaction

Author

Marta, M., Formicola, A., Gyurky, Gy., Bemmerer, D., Broggini, C., Caciolli, A., Corvisiero, P., Costantini, H., Elekes, Z., Fulop, Zs., Gervino, G., Guglielmetti, A., Gustavino, C., Imbriani, G., Junker, M., Kunz, R., Lemut, A., Limata, B., Mazzocchi, C., Menegazzo, R., Prati, P., Roca, V., Rolfs, C., Romano, M., Alvarez, C. Rossi, Somorjai, E., Straniero, O., Strieder, F., Terrasi, F., Trautvetter, H. P., Vomiero, A., Marta, M., Formicola, A., Gyurky, Gy., Bemmerer, D., Broggini, C., Caciolli, A., Corvisiero, P., Costantini, H., Elekes, Z., Fulop, Zs., Gervino, G., Guglielmetti, A., Gustavino, C., Imbriani, G., Junker, M., Kunz, R., Lemut, A., Limata, B., Mazzocchi, C., Menegazzo, R., Prati, P., Roca, V., Rolfs, C., Romano, M., Alvarez, C. Rossi, Somorjai, E., Straniero, O., Strieder, F., Terrasi, F., Trautvetter, H. P., and Vomiero, A.

Abstract

The rate of the hydrogen-burning carbon-nitrogen-oxygen (CNO) cycle is controlled by the slowest process, 14N(p,gamma)15O, which proceeds by capture to the ground and several excited states in 15O. Previous extrapolations for the ground state contribution disagreed by a factor 2, corresponding to 15% uncertainty in the total astrophysical S-factor. At the Laboratory for Underground Nuclear Astrophysics (LUNA) 400 kV accelerator placed deep underground in the Gran Sasso facility in Italy, a new experiment on ground state capture has been carried out at 317.8, 334.4, and 353.3 keV center-of-mass energy. Systematic corrections have been reduced considerably with respect to previous studies by using a Clover detector and by adopting a relative analysis. The previous discrepancy has been resolved, and ground state capture no longer dominates the uncertainty of the total S-factor., Comment: Phys. Rev. C, rapid comm., accepted

Published
2008
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9. Precision study of ground state capture in the 14N(p,gamma)15O reaction

Author

Marta, M., Formicola, A., Gyurky, Gy., Bemmerer, D., Broggini, C., Caciolli, A., Corvisiero, P., Costantini, H., Elekes, Z., Fulop, Zs., Gervino, G., Guglielmetti, A., Gustavino, C., Imbriani, G., Junker, M., Kunz, R., Lemut, A., Limata, B., Mazzocchi, C., Menegazzo, R., Prati, P., Roca, V., Rolfs, C., Romano, M., Alvarez, C. Rossi, Somorjai, E., Straniero, O., Strieder, F., Terrasi, F., Trautvetter, H. P., Vomiero, A., Marta, M., Formicola, A., Gyurky, Gy., Bemmerer, D., Broggini, C., Caciolli, A., Corvisiero, P., Costantini, H., Elekes, Z., Fulop, Zs., Gervino, G., Guglielmetti, A., Gustavino, C., Imbriani, G., Junker, M., Kunz, R., Lemut, A., Limata, B., Mazzocchi, C., Menegazzo, R., Prati, P., Roca, V., Rolfs, C., Romano, M., Alvarez, C. Rossi, Somorjai, E., Straniero, O., Strieder, F., Terrasi, F., Trautvetter, H. P., and Vomiero, A.

Abstract

The rate of the hydrogen-burning carbon-nitrogen-oxygen (CNO) cycle is controlled by the slowest process, 14N(p,gamma)15O, which proceeds by capture to the ground and several excited states in 15O. Previous extrapolations for the ground state contribution disagreed by a factor 2, corresponding to 15% uncertainty in the total astrophysical S-factor. At the Laboratory for Underground Nuclear Astrophysics (LUNA) 400 kV accelerator placed deep underground in the Gran Sasso facility in Italy, a new experiment on ground state capture has been carried out at 317.8, 334.4, and 353.3 keV center-of-mass energy. Systematic corrections have been reduced considerably with respect to previous studies by using a Clover detector and by adopting a relative analysis. The previous discrepancy has been resolved, and ground state capture no longer dominates the uncertainty of the total S-factor., Comment: Phys. Rev. C, rapid comm., accepted

Published
2008
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10. 3He(alpha,gamma)7Be cross section at low energies

Author

Gyurky, Gy., Confortola, F., Costantini, H., Formicola, A., Bemmerer, D., Bonetti, R., Broggini, C., Corvisiero, P., Elekes, Z., Fulop, Zs., Gervino, G., Guglielmetti, A., Gustavino, C., Imbriani, G., Junker, M., Laubenstein, M., Lemut, A., Limata, B., Lozza, V., Marta, M., Menegazzo, R., Prati, P., Roca, V., Rolfs, C., Alvarez, C. Rossi, Somorjai, E., Straniero, O., Strieder, F., Terrasi, F., Trautvetter, H. P., Gyurky, Gy., Confortola, F., Costantini, H., Formicola, A., Bemmerer, D., Bonetti, R., Broggini, C., Corvisiero, P., Elekes, Z., Fulop, Zs., Gervino, G., Guglielmetti, A., Gustavino, C., Imbriani, G., Junker, M., Laubenstein, M., Lemut, A., Limata, B., Lozza, V., Marta, M., Menegazzo, R., Prati, P., Roca, V., Rolfs, C., Alvarez, C. Rossi, Somorjai, E., Straniero, O., Strieder, F., Terrasi, F., and Trautvetter, H. P.

Abstract

The flux of 7Be and 8B neutrinos from the Sun and the production of 7Li via primordial nucleosynthesis depend on the rate of the 3He(alpha,gamma)7Be reaction. In extension of a previous study showing cross section data at 127 - 167 keV center of mass energy, the present work reports on a measurement of the 3He(alpha,gamma)7Be cross section at 106 keV performed at Italy's Gran Sasso underground laboratory by the activation method. This energy is closer to the solar Gamow energy than ever reached before. The result is sigma = 0.567 +- 0.029(stat) +- 0.016(syst) nbarn. The data are compared with previous activation studies at high energy, and a recommended S(0) value for all 3He(alpha,gamma)7Be activation studies, including the present work, is given., Comment: Accepted for publication in PRC

Published
2007
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11. 3He(alpha,gamma)7Be cross section at low energies

Author

Gyurky, Gy., Confortola, F., Costantini, H., Formicola, A., Bemmerer, D., Bonetti, R., Broggini, C., Corvisiero, P., Elekes, Z., Fulop, Zs., Gervino, G., Guglielmetti, A., Gustavino, C., Imbriani, G., Junker, M., Laubenstein, M., Lemut, A., Limata, B., Lozza, V., Marta, M., Menegazzo, R., Prati, P., Roca, V., Rolfs, C., Alvarez, C. Rossi, Somorjai, E., Straniero, O., Strieder, F., Terrasi, F., Trautvetter, H. P., Gyurky, Gy., Confortola, F., Costantini, H., Formicola, A., Bemmerer, D., Bonetti, R., Broggini, C., Corvisiero, P., Elekes, Z., Fulop, Zs., Gervino, G., Guglielmetti, A., Gustavino, C., Imbriani, G., Junker, M., Laubenstein, M., Lemut, A., Limata, B., Lozza, V., Marta, M., Menegazzo, R., Prati, P., Roca, V., Rolfs, C., Alvarez, C. Rossi, Somorjai, E., Straniero, O., Strieder, F., Terrasi, F., and Trautvetter, H. P.

Abstract

The flux of 7Be and 8B neutrinos from the Sun and the production of 7Li via primordial nucleosynthesis depend on the rate of the 3He(alpha,gamma)7Be reaction. In extension of a previous study showing cross section data at 127 - 167 keV center of mass energy, the present work reports on a measurement of the 3He(alpha,gamma)7Be cross section at 106 keV performed at Italy's Gran Sasso underground laboratory by the activation method. This energy is closer to the solar Gamow energy than ever reached before. The result is sigma = 0.567 +- 0.029(stat) +- 0.016(syst) nbarn. The data are compared with previous activation studies at high energy, and a recommended S(0) value for all 3He(alpha,gamma)7Be activation studies, including the present work, is given., Comment: Accepted for publication in PRC

Published
2007
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12. Activation measurement of the 3He(alpha,gamma)7Be cross section at low energy

Author

Bemmerer, D., Confortola, F., Costantini, H., Formicola, A., Gyurky, Gy., Bonetti, R., Broggini, C., Corvisiero, P., Elekes, Z., Fulop, Zs., Gervino, G., Guglielmetti, A., Gustavino, C., Imbriani, G., Junker, M., Laubenstein, M., Lemut, A., Limata, B., Lozza, V., Marta, M., Menegazzo, R., Prati, P., Roca, V., Rolfs, C., Alvarez, C. Rossi, Somorjai, E., Straniero, O., Strieder, F., Terrasi, F., Trautvetter, H. P., Bemmerer, D., Confortola, F., Costantini, H., Formicola, A., Gyurky, Gy., Bonetti, R., Broggini, C., Corvisiero, P., Elekes, Z., Fulop, Zs., Gervino, G., Guglielmetti, A., Gustavino, C., Imbriani, G., Junker, M., Laubenstein, M., Lemut, A., Limata, B., Lozza, V., Marta, M., Menegazzo, R., Prati, P., Roca, V., Rolfs, C., Alvarez, C. Rossi, Somorjai, E., Straniero, O., Strieder, F., Terrasi, F., and Trautvetter, H. P.

Abstract

The nuclear physics input from the 3He(alpha,gamma)7Be cross section is a major uncertainty in the fluxes of 7Be and 8B neutrinos from the Sun predicted by solar models and in the 7Li abundance obtained in big-bang nucleosynthesis calculations. The present work reports on a new precision experiment using the activation technique at energies directly relevant to big-bang nucleosynthesis. Previously such low energies had been reached experimentally only by the prompt-gamma technique and with inferior precision. Using a windowless gas target, high beam intensity and low background gamma-counting facilities, the 3He(alpha,gamma)7Be cross section has been determined at 127, 148 and 169 keV center-of-mass energy with a total uncertainty of 4%. The sources of systematic uncertainty are discussed in detail. The present data can be used in big-bang nucleosynthesis calculations and to constrain the extrapolation of the 3He(alpha,gamma)7Be astrophysical S-factor to solar energies.

Published
2006
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13. First measurement of the 14N(p,gamma)15O cross section down to 70 keV

Author

Lemut, A., Bemmerer, D., Confortola, F., Bonetti, R., Broggini, C., Corvisiero, P., Costantini, H., Cruz, J., Formicola, A., Fulop, Zs., Gervino, G., Guglielmetti, A., Gustavino, C., Gyurky, Gy., Imbriani, G., Jesus, A. P., Junker, M., Limata, B., Menegazzo, R., Prati, P., Roca, V., Rogalla, D., Rolfs, C., Romano, M., Alvarez, C. Rossi, Schumann, F., Somorjai, E., Straniero, O., Strieder, F., Terrasi, F., Trautvetter, H. P., Lemut, A., Bemmerer, D., Confortola, F., Bonetti, R., Broggini, C., Corvisiero, P., Costantini, H., Cruz, J., Formicola, A., Fulop, Zs., Gervino, G., Guglielmetti, A., Gustavino, C., Gyurky, Gy., Imbriani, G., Jesus, A. P., Junker, M., Limata, B., Menegazzo, R., Prati, P., Roca, V., Rogalla, D., Rolfs, C., Romano, M., Alvarez, C. Rossi, Schumann, F., Somorjai, E., Straniero, O., Strieder, F., Terrasi, F., and Trautvetter, H. P.

Abstract

In stars with temperatures above 20*10^6 K, hydrogen burning is dominated by the CNO cycle. Its rate is determined by the slowest process, the 14N(p,gamma)15O reaction. Deep underground in Italy's Gran Sasso laboratory, at the LUNA 400 kV accelerator, the cross section of this reaction has been measured at energies much lower than ever achieved before. Using a windowless gas target and a 4pi BGO summing detector, direct cross section data has been obtained down to 70 keV, reaching a value of 0.24 picobarn. The Gamow peak has been covered by experimental data for several scenarios of stable and explosive hydrogen burning. In addition, the strength of the 259 keV resonance has been remeasured. The thermonuclear reaction rate has been calculated for temperatures 90 - 300 *10^6 K, for the first time with negligible impact from extrapolations.

Published
2006
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14. Activation measurement of the 3He(alpha,gamma)7Be cross section at low energy

Author

Bemmerer, D., Confortola, F., Costantini, H., Formicola, A., Gyurky, Gy., Bonetti, R., Broggini, C., Corvisiero, P., Elekes, Z., Fulop, Zs., Gervino, G., Guglielmetti, A., Gustavino, C., Imbriani, G., Junker, M., Laubenstein, M., Lemut, A., Limata, B., Lozza, V., Marta, M., Menegazzo, R., Prati, P., Roca, V., Rolfs, C., Alvarez, C. Rossi, Somorjai, E., Straniero, O., Strieder, F., Terrasi, F., Trautvetter, H. P., Bemmerer, D., Confortola, F., Costantini, H., Formicola, A., Gyurky, Gy., Bonetti, R., Broggini, C., Corvisiero, P., Elekes, Z., Fulop, Zs., Gervino, G., Guglielmetti, A., Gustavino, C., Imbriani, G., Junker, M., Laubenstein, M., Lemut, A., Limata, B., Lozza, V., Marta, M., Menegazzo, R., Prati, P., Roca, V., Rolfs, C., Alvarez, C. Rossi, Somorjai, E., Straniero, O., Strieder, F., Terrasi, F., and Trautvetter, H. P.

Abstract

The nuclear physics input from the 3He(alpha,gamma)7Be cross section is a major uncertainty in the fluxes of 7Be and 8B neutrinos from the Sun predicted by solar models and in the 7Li abundance obtained in big-bang nucleosynthesis calculations. The present work reports on a new precision experiment using the activation technique at energies directly relevant to big-bang nucleosynthesis. Previously such low energies had been reached experimentally only by the prompt-gamma technique and with inferior precision. Using a windowless gas target, high beam intensity and low background gamma-counting facilities, the 3He(alpha,gamma)7Be cross section has been determined at 127, 148 and 169 keV center-of-mass energy with a total uncertainty of 4%. The sources of systematic uncertainty are discussed in detail. The present data can be used in big-bang nucleosynthesis calculations and to constrain the extrapolation of the 3He(alpha,gamma)7Be astrophysical S-factor to solar energies.

Published
2006
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15. First measurement of the 14N(p,gamma)15O cross section down to 70 keV

Author

Lemut, A., Bemmerer, D., Confortola, F., Bonetti, R., Broggini, C., Corvisiero, P., Costantini, H., Cruz, J., Formicola, A., Fulop, Zs., Gervino, G., Guglielmetti, A., Gustavino, C., Gyurky, Gy., Imbriani, G., Jesus, A. P., Junker, M., Limata, B., Menegazzo, R., Prati, P., Roca, V., Rogalla, D., Rolfs, C., Romano, M., Alvarez, C. Rossi, Schumann, F., Somorjai, E., Straniero, O., Strieder, F., Terrasi, F., Trautvetter, H. P., Lemut, A., Bemmerer, D., Confortola, F., Bonetti, R., Broggini, C., Corvisiero, P., Costantini, H., Cruz, J., Formicola, A., Fulop, Zs., Gervino, G., Guglielmetti, A., Gustavino, C., Gyurky, Gy., Imbriani, G., Jesus, A. P., Junker, M., Limata, B., Menegazzo, R., Prati, P., Roca, V., Rogalla, D., Rolfs, C., Romano, M., Alvarez, C. Rossi, Schumann, F., Somorjai, E., Straniero, O., Strieder, F., Terrasi, F., and Trautvetter, H. P.

Abstract

In stars with temperatures above 20*10^6 K, hydrogen burning is dominated by the CNO cycle. Its rate is determined by the slowest process, the 14N(p,gamma)15O reaction. Deep underground in Italy's Gran Sasso laboratory, at the LUNA 400 kV accelerator, the cross section of this reaction has been measured at energies much lower than ever achieved before. Using a windowless gas target and a 4pi BGO summing detector, direct cross section data has been obtained down to 70 keV, reaching a value of 0.24 picobarn. The Gamow peak has been covered by experimental data for several scenarios of stable and explosive hydrogen burning. In addition, the strength of the 259 keV resonance has been remeasured. The thermonuclear reaction rate has been calculated for temperatures 90 - 300 *10^6 K, for the first time with negligible impact from extrapolations.

Published
2006
Full Text
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16. Elastic alpha-scattering of 112Sn and 124Sn at astrophysically relevant energies

Author

Galaviz, D., Fulop, Zs., Gyurky, Gy., Mate, Z., Mohr, P., Rauscher, T., Somorjai, E., Zilges, A., Galaviz, D., Fulop, Zs., Gyurky, Gy., Mate, Z., Mohr, P., Rauscher, T., Somorjai, E., and Zilges, A.

Abstract

The cross sections for the elastic scattering reactions {112,124}Sn(a,a){112,124}Sn at energies above and below the Coulomb barrier are presented and compared to predictions for global alpha-nucleus potentials. The high precision of the new data allows a study of the global alpha-nucleus potentials at both the proton and neutron-rich sides of an isotopic chain. In addition, local alpha-nucleus potentials have been extracted for both nuclei, and used to reproduce elastic scattering data at higher energies. Predictions from the capture cross section of the reaction 112Sn(a,g)116Te at astrophysically relevant energies are presented and compared to experimental data., Comment: 20 pages, 10 figures, accepted for publication in Phys. Rev. C

Published
2005
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17. S-factor of 14N(p,Y)15O at astrophysical energies

Author

Imbriana, G., Costantini, H., Formicola, A., Vomiero, A., Angulo Perez, Carmen, Bemmerer, D., Bonetti, R., Broggini, C., Confortola, F., Corvisiero, P., Cruz, J., Descouvemont, Pierre, Fulop, Zsolt, Gervino, G., Guglielmetti, A., Gustavino, C., Gyurky, Gy, Jesus, A. P., Junker, Matthias, Klug, J. N., Lemut, A., Menegazzo, R., Prati, R., Roca, V., Rolfs, Claus, Romano, M., lvarez, C., Schümann, F., Schürmann, D., Somorjai, Endre, Straniero, O., Strieder, Frank, Terrasi, F., Trauvetter, H. P., Imbriana, G., Costantini, H., Formicola, A., Vomiero, A., Angulo Perez, Carmen, Bemmerer, D., Bonetti, R., Broggini, C., Confortola, F., Corvisiero, P., Cruz, J., Descouvemont, Pierre, Fulop, Zsolt, Gervino, G., Guglielmetti, A., Gustavino, C., Gyurky, Gy, Jesus, A. P., Junker, Matthias, Klug, J. N., Lemut, A., Menegazzo, R., Prati, R., Roca, V., Rolfs, Claus, Romano, M., lvarez, C., Schümann, F., Schürmann, D., Somorjai, Endre, Straniero, O., Strieder, Frank, Terrasi, F., and Trauvetter, H. P.

Abstract

info:eu-repo/semantics/published

Published
2005

18. S-factor of 14N(p,Y)15O at astrophysical energies

Author

Imbriana, G., Costantini, H., Formicola, A., Vomiero, A., Angulo Perez, Carmen, Bemmerer, D., Bonetti, R., Broggini, C., Confortola, F., Corvisiero, P., Cruz, J., Descouvemont, Pierre, Fulop, Zsolt, Gervino, G., Guglielmetti, A., Gustavino, C., Gyurky, Gy, Jesus, A. P., Junker, Matthias, Klug, J. N., Lemut, A., Menegazzo, R., Prati, R., Roca, V., Rolfs, Claus, Romano, M., lvarez, C., Schümann, F., Schürmann, D., Somorjai, Endre, Straniero, O., Strieder, Frank, Terrasi, F., Trauvetter, H. P., Imbriana, G., Costantini, H., Formicola, A., Vomiero, A., Angulo Perez, Carmen, Bemmerer, D., Bonetti, R., Broggini, C., Confortola, F., Corvisiero, P., Cruz, J., Descouvemont, Pierre, Fulop, Zsolt, Gervino, G., Guglielmetti, A., Gustavino, C., Gyurky, Gy, Jesus, A. P., Junker, Matthias, Klug, J. N., Lemut, A., Menegazzo, R., Prati, R., Roca, V., Rolfs, Claus, Romano, M., lvarez, C., Schümann, F., Schürmann, D., Somorjai, Endre, Straniero, O., Strieder, Frank, Terrasi, F., and Trauvetter, H. P.

Abstract

info:eu-repo/semantics/published

Published
2005

19. Elastic alpha-scattering of 112Sn and 124Sn at astrophysically relevant energies

Author

Galaviz, D., Fulop, Zs., Gyurky, Gy., Mate, Z., Mohr, P., Rauscher, T., Somorjai, E., Zilges, A., Galaviz, D., Fulop, Zs., Gyurky, Gy., Mate, Z., Mohr, P., Rauscher, T., Somorjai, E., and Zilges, A.

Abstract

The cross sections for the elastic scattering reactions {112,124}Sn(a,a){112,124}Sn at energies above and below the Coulomb barrier are presented and compared to predictions for global alpha-nucleus potentials. The high precision of the new data allows a study of the global alpha-nucleus potentials at both the proton and neutron-rich sides of an isotopic chain. In addition, local alpha-nucleus potentials have been extracted for both nuclei, and used to reproduce elastic scattering data at higher energies. Predictions from the capture cross section of the reaction 112Sn(a,g)116Te at astrophysically relevant energies are presented and compared to experimental data., Comment: 20 pages, 10 figures, accepted for publication in Phys. Rev. C

Published
2005
Full Text
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20. Astrophysical S-factor of 14N(p,)15O

Author

Formicola, A., Imbriana, G., Costantini, H., Angulo Perez, Carmen, Bemmerer, D., Bonetti, R., Broggini, C., Corvisiero, P., Cruz, J., Descouvemont, Pierre, Fulop, Zsolt, Gervino, G., Guglielmetti, A., Gustavino, C., Gyurky, Gy, Jesus, A. P., Junker, Matthias, Lemut, A., Menegazzo, R., Prati, P., Roca, V., Rolfs, Claus, Romano, M., Alvarez, C., Schumann, F., Somorjai, Endre, Straniero, O., Strieder, Frank, Terrasi, F., Trautvetter, H. P., Vomiero, A., Zavatarelli, Sandra, Formicola, A., Imbriana, G., Costantini, H., Angulo Perez, Carmen, Bemmerer, D., Bonetti, R., Broggini, C., Corvisiero, P., Cruz, J., Descouvemont, Pierre, Fulop, Zsolt, Gervino, G., Guglielmetti, A., Gustavino, C., Gyurky, Gy, Jesus, A. P., Junker, Matthias, Lemut, A., Menegazzo, R., Prati, P., Roca, V., Rolfs, Claus, Romano, M., Alvarez, C., Schumann, F., Somorjai, Endre, Straniero, O., Strieder, Frank, Terrasi, F., Trautvetter, H. P., Vomiero, A., and Zavatarelli, Sandra

Abstract

We report on a new measurement of the 14N(p,γ) 15O capture cross section at Ep=140 to 400 keV using the 400 kV LUNA accelerator facility at the Laboratori Nazionali del Gran Sasso (LNGS). The uncertainties have been reduced with respect to previous measurements and their analysis. We have analyzed the data using the R-matrix method and we find that the ground state transition accounts for about 15% of the total S-factor. The main contribution to the S-factor is given by the transition to the 6.79 MeV state. We find a total S(0)=1.7±0.2 keVb, in agreement with recent extrapolations. The result has important consequences for the solar neutrino spectrum as well as for the age of globular clusters. © 2004 Elsevier B.V. All rights reserved., info:eu-repo/semantics/published

Published
2004

21. Se(p-γ) cross section measurements for p-process studies

Author

Gyurky, Gy, Fulop, Zsolt, Somorjai, Endre, Elekes, Zoltán, Kokkoris, Michael, Galanopulos, S., Demetriou, Paraskevi, Harissopulos, Sotirios, Goriely, Stéphane, Rauscher, Thomas, Gyurky, Gy, Fulop, Zsolt, Somorjai, Endre, Elekes, Zoltán, Kokkoris, Michael, Galanopulos, S., Demetriou, Paraskevi, Harissopulos, Sotirios, Goriely, Stéphane, and Rauscher, Thomas

Abstract

As a continuation of a systematic study of reactions relevant to astrophysical p-process, the (p,γ) or (p.n) cross sections of three Se isotopes have been measured using an activation technique in the proton energy range between 1.3 and 3.6 MeV. The resulting cross sections of the 74,76Se(p,γ)75,77Br and 82Se(p,n)82Br reaction have been conipared with the predictions of Hauser-Feshbach statistical model calculations using the NON-SMOKER and MOST codes. In all three cases the theory is in satisfactory agreement with the measurements., SCOPUS: ar.j, info:eu-repo/semantics/published

Published
2003

22. The 88Sr(p, γ)89Y reaction at astrophysically relevant energies

Author

Galanopulos, S., Demetriou, Paraskevi, Kokkoris, Michael, Harissopulos, Sotirios, Kunz, Rino, Fey, M., Hammer, Johann Wolfgang, Gyurky, Gy, Fulop, Zsolt, Somorjai, Endre, Goriely, Stéphane, Galanopulos, S., Demetriou, Paraskevi, Kokkoris, Michael, Harissopulos, Sotirios, Kunz, Rino, Fey, M., Hammer, Johann Wolfgang, Gyurky, Gy, Fulop, Zsolt, Somorjai, Endre, and Goriely, Stéphane

Abstract

SCOPUS: ar.j, info:eu-repo/semantics/published

Published
2003

23. A systematic study of proton capture reactions in the Se-Sb region at energies relevant to the p process

Author

Harissopulos, Sotirios, Galanopulos, S., Demetriou, Paraskevi, Spyrou, Artemis, Kriembardis, G., Kokkoris, Michael, Karydas, Andreas Germanos, Zarkadas, Ch, Kunz, Rino, Fey, M., Hammer, Johann Wolfgang, Gyurky, Gy, Fulop, Zsolt, Somorjai, Endre, Dewald, Alfred, Zell, Karl Oskar, von Brentano, Peter, Julin, Rauno, Goriely, Stéphane, Harissopulos, Sotirios, Galanopulos, S., Demetriou, Paraskevi, Spyrou, Artemis, Kriembardis, G., Kokkoris, Michael, Karydas, Andreas Germanos, Zarkadas, Ch, Kunz, Rino, Fey, M., Hammer, Johann Wolfgang, Gyurky, Gy, Fulop, Zsolt, Somorjai, Endre, Dewald, Alfred, Zell, Karl Oskar, von Brentano, Peter, Julin, Rauno, and Goriely, Stéphane

Abstract

A systematic investigation of (p,γ) cross sections of nuclei from Se to Sb is presented. In-beam cross section measurements were carried out at Ep=1.4-5 MeV by using an array of 4 HPGe detectors of 100% relative efficiency shielded with BGO crystals. The S factors obtained are compared with the predictions of the statistical model code MOST., SCOPUS: ar.j, info:eu-repo/semantics/published

Published
2003

24. The [Formula Presented] reaction at astrophysically relevant energies

Author

Galanopoulos, S., Somorjai, Endre, Goriely, Stéphane, Demetriou, Paraskevi, Kokkoris, Michael, Harissopulos, Sotirios, Kunz, Rino, Fey, M., Hammer, Johann Wolfgang, Gyurky, Gy, Fulop, Zsolt, Galanopoulos, S., Somorjai, Endre, Goriely, Stéphane, Demetriou, Paraskevi, Kokkoris, Michael, Harissopulos, Sotirios, Kunz, Rino, Fey, M., Hammer, Johann Wolfgang, Gyurky, Gy, and Fulop, Zsolt

Abstract

The cross section of the [Formula Presented] reaction was determined by in-beam measurements at energies [Formula Presented] relevant to the nucleosynthetic p process. At [Formula Presented] the γ angular distributions were obtained by using one HPGe detector of 80% relative efficiency, whereas at [Formula Presented] they were measured by means of an array of four HPGe detectors all shielded with BGO crystals for Compton background supression. Three of them had a relative efficiency [Formula Presented] whereas the remaining one had [Formula Presented] From the resulting cross sections, that lie in the 0.5-μb–5-mb range, astrophysical S factors and reaction rates have been derived. Cross sections, S factors, and reaction rates have also been calculated by means of the statistical model code MOST. A very good agreement between the experimental data and the theoretical predictions has been found. © 2003 The American Physical Society., SCOPUS: ar.j, info:eu-repo/semantics/published

Published
2003

25. Proton induced reaction cross section measurements on Se isotopes for the astrophysical p-process

Author

Gyurky, Gy, Fulop, Zsolt, Somorjai, Endre, Kokkoris, Michael, Galanopulos, S., Demetriou, Paraskevi, Harissopulos, Sotirios, Rauscher, Thomas, Goriely, Stéphane, Gyurky, Gy, Fulop, Zsolt, Somorjai, Endre, Kokkoris, Michael, Galanopulos, S., Demetriou, Paraskevi, Harissopulos, Sotirios, Rauscher, Thomas, and Goriely, Stéphane

Abstract

info:eu-repo/semantics/published

Published
2003

26. A systematic study of proton-capture cross sections in the Se-Sb region with relevance to the p-process nucleosynthesis

Author

Harissopulos, Sotirios, Demetriou, Paraskevi, Galanopulos, S., Kokkoris, Michael, Kriembardis, G., Tsagari, P., Spyrou, Artemis, Kalyva, G., Zakadas, C., Karydas, Andreas Germanos, Hammer, Johann Wolfgang, Kunz, Rino, Fey, M., Somorjai, Endre, Gyurky, Gy, Fulop, Zsolt, Dewald, Alfred, Zell, Karl Oskar, von Brentano, Peter, Julin, Rauno, Goriely, Stéphane, Harissopulos, Sotirios, Demetriou, Paraskevi, Galanopulos, S., Kokkoris, Michael, Kriembardis, G., Tsagari, P., Spyrou, Artemis, Kalyva, G., Zakadas, C., Karydas, Andreas Germanos, Hammer, Johann Wolfgang, Kunz, Rino, Fey, M., Somorjai, Endre, Gyurky, Gy, Fulop, Zsolt, Dewald, Alfred, Zell, Karl Oskar, von Brentano, Peter, Julin, Rauno, and Goriely, Stéphane

Abstract

info:eu-repo/semantics/published

Published
2003

27. Proton induced reaction cross section measurements on Se isotopes for the astrophysical p-process

Author

Gyurky, Gy, Fulop, Zsolt, Somorjai, Endre, Kokkoris, Michael, Galanopulos, S., Demetriou, Paraskevi, Harissopulos, Sotirios, Rauscher, Thomas, Goriely, Stéphane, Gyurky, Gy, Fulop, Zsolt, Somorjai, Endre, Kokkoris, Michael, Galanopulos, S., Demetriou, Paraskevi, Harissopulos, Sotirios, Rauscher, Thomas, and Goriely, Stéphane

Abstract

info:eu-repo/semantics/published

Published
2003

28. Se(p,gamma) cross section measurements for p-process studies

Author

Gyurky, Gy, Fulop, Zsolt, Somorjai, Endre, Kokkoris, Michael, Galanopulos, S., Demetriou, Paraskevi, Harissopulos, Sotirios, Goriely, Stéphane, Rauscher, Thomas, Gyurky, Gy, Fulop, Zsolt, Somorjai, Endre, Kokkoris, Michael, Galanopulos, S., Demetriou, Paraskevi, Harissopulos, Sotirios, Goriely, Stéphane, and Rauscher, Thomas

Abstract

info:eu-repo/semantics/published

Published
2003

29. A systematic study of proton-capture cross sections in the Se-Sb region with relevance to the p-process nucleosynthesis

Author

Harissopulos, Sotirios, Demetriou, Paraskevi, Galanopulos, S., Kokkoris, Michael, Kriembardis, G., Tsagari, P., Spyrou, Artemis, Kalyva, G., Zakadas, C., Karydas, Andreas Germanos, Hammer, Johann Wolfgang, Kunz, Rino, Fey, M., Somorjai, Endre, Gyurky, Gy, Fulop, Zsolt, Dewald, Alfred, Zell, Karl Oskar, von Brentano, Peter, Julin, Rauno, Goriely, Stéphane, Harissopulos, Sotirios, Demetriou, Paraskevi, Galanopulos, S., Kokkoris, Michael, Kriembardis, G., Tsagari, P., Spyrou, Artemis, Kalyva, G., Zakadas, C., Karydas, Andreas Germanos, Hammer, Johann Wolfgang, Kunz, Rino, Fey, M., Somorjai, Endre, Gyurky, Gy, Fulop, Zsolt, Dewald, Alfred, Zell, Karl Oskar, von Brentano, Peter, Julin, Rauno, and Goriely, Stéphane

Abstract

info:eu-repo/semantics/published

Published
2003

30. Proton induced reaction cross section measurements on Se isotopes for the astrophysical [Formula Presented] process

Author

Gyurky, Gy, Fulop, Zsolt, Somorjai, Endre, Kokkoris, Michael, Galanopoulos, S., Demetriou, Paraskevi, Harissopulos, Sotirios, Rauscher, Thomas, Goriely, Stéphane, Gyurky, Gy, Fulop, Zsolt, Somorjai, Endre, Kokkoris, Michael, Galanopoulos, S., Demetriou, Paraskevi, Harissopulos, Sotirios, Rauscher, Thomas, and Goriely, Stéphane

Abstract

As a continuation of a systematic study of reactions relevant to the astrophysical [Formula Presented] process, the cross sections of the [Formula Presented] and [Formula Presented] reactions have been measured at energies from 1.3 to [Formula Presented] using an activation technique. The results are compared to the predictions of Hauser-Feshbach statistical model calculations using the NON-SMOKER and MOST codes. The sensitivity of the calculations to variations in the optical proton potential and the nuclear level density was studied. Good agreement between theoretical and experimental reaction rates was found for the reactions [Formula Presented] and [Formula Presented]. © 2003 The American Physical Society., SCOPUS: ar.j, info:eu-repo/semantics/published

Published
2003

31. Cross sections of (p, γ) reactions of N = 50 nuclei relevant to p-process

Author

Harissopulos, Sotirios, Somorjai, Endre, Goriely, Stéphane, Kasemann, S., Dewald, Alfred, Zell, Karl Oskar, Galanopoulos, S., Tsagari, P., Demetriou, Paraskevi, Kuburas, G., Paradellis, Th, Kunz, Rino, Hammer, Josef Wolfgang, Gyurky, Gy, Harissopulos, Sotirios, Somorjai, Endre, Goriely, Stéphane, Kasemann, S., Dewald, Alfred, Zell, Karl Oskar, Galanopoulos, S., Tsagari, P., Demetriou, Paraskevi, Kuburas, G., Paradellis, Th, Kunz, Rino, Hammer, Josef Wolfgang, and Gyurky, Gy

Abstract

The proton capture reactions 89Y(p,γ)90Zr and 88Sr(p,γ)89Y have been investigated at energies Ep = 1.5-3.5 MeV via an array of 4 HPGe detectors of ≈100% rel. efficiency. The resulting cross sections as well as the existing data on the 90Zr(p,γ)91Nb and 92Mo(p,γ)93Tc reactions are compared with improved statistical model calculations carried out using the MOST code., SCOPUS: ar.j, info:eu-repo/semantics/published

Published
2001

32. Cross sections of (p,gamma) reactions of N=50 nuclei relevant to p-process

Author

Harissopulos, Sotirios, Galanopulos, S., Tsagari, P., Demetriou, Paraskevi, Kuburas, G., Paradellis, Th, Kunz, Rino, Hammer, Johann Wolfgang, Gyurky, Gy, Somorjai, Endre, Goriely, Stéphane, Kasemann, S., Dewald, Alfred, Zelle, K.O., Harissopulos, Sotirios, Galanopulos, S., Tsagari, P., Demetriou, Paraskevi, Kuburas, G., Paradellis, Th, Kunz, Rino, Hammer, Johann Wolfgang, Gyurky, Gy, Somorjai, Endre, Goriely, Stéphane, Kasemann, S., Dewald, Alfred, and Zelle, K.O.

Abstract

info:eu-repo/semantics/published

Published
2001

33. Cross sections of (p,gamma) reactions of N=50 nuclei relevant to p-process

Author

Harissopulos, Sotirios, Galanopulos, S., Tsagari, P., Demetriou, Paraskevi, Kuburas, G., Paradellis, Th, Kunz, Rino, Hammer, Johann Wolfgang, Gyurky, Gy, Somorjai, Endre, Goriely, Stéphane, Kasemann, S., Dewald, Alfred, Zelle, K.O., Harissopulos, Sotirios, Galanopulos, S., Tsagari, P., Demetriou, Paraskevi, Kuburas, G., Paradellis, Th, Kunz, Rino, Hammer, Johann Wolfgang, Gyurky, Gy, Somorjai, Endre, Goriely, Stéphane, Kasemann, S., Dewald, Alfred, and Zelle, K.O.

Abstract

info:eu-repo/semantics/published

Published
2001

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