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First direct measurement of the 64.5 keV resonance strength in $^{17}$O(p,$γ$)$^{18}$F reaction

Fuente: arXiv

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Détails bibliographiques
Auteurs principaux:	Gesuè, R. M., Ciani, G. F., Piatti, D., Boeltzig, A., Rapagnani, D., Aliotta, M., Ananna, C., Barbieri, L., Barile, F., Bemmerer, D., Best, A., Broggini, C., Bruno, C. G., Caciolli, A., Campostrini, M., Casaburo, F., Cavanna, F., Colombetti, P., Compagnucci, A., Corvisiero, P., Csedreki, L., Davinson, T., De Gregorio, G. M., Dell'Aquila, D., Depalo, R., Di Leva, A., Elekes, Z., Ferraro, F., Formicola, A., Fülöp, Zs., Gervino, G., Guglielmetti, A., Gustavino, C., Gyürky, Gy., Imbriani, G., Junker, M., Lugaro, M., Marigo, P., Marsh, J., Masha, E., Menegazzo, R., Mercogliano, D., Paticchio, V., Perrino, R., Prati, P., Rigato, V., Robb, D., Schiavulli, L., Sidhu, R. S., Skowronski, J., Straniero, O., Szücs, T., Zavatarelli, S.
Format:	Preprint
Publié:	2024
Sujets:	Nuclear Experiment
Accès en ligne:	Acceder al recurso
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_version_	1866914902661136384
author	Gesuè, R. M. Ciani, G. F. Piatti, D. Boeltzig, A. Rapagnani, D. Aliotta, M. Ananna, C. Barbieri, L. Barile, F. Bemmerer, D. Best, A. Broggini, C. Bruno, C. G. Caciolli, A. Campostrini, M. Casaburo, F. Cavanna, F. Colombetti, P. Compagnucci, A. Corvisiero, P. Csedreki, L. Davinson, T. De Gregorio, G. M. Dell'Aquila, D. Depalo, R. Di Leva, A. Elekes, Z. Ferraro, F. Formicola, A. Fülöp, Zs. Gervino, G. Guglielmetti, A. Gustavino, C. Gyürky, Gy. Imbriani, G. Junker, M. Lugaro, M. Marigo, P. Marsh, J. Masha, E. Menegazzo, R. Mercogliano, D. Paticchio, V. Perrino, R. Prati, P. Rigato, V. Robb, D. Schiavulli, L. Sidhu, R. S. Skowronski, J. Straniero, O. Szücs, T. Zavatarelli, S.
author_facet	Gesuè, R. M. Ciani, G. F. Piatti, D. Boeltzig, A. Rapagnani, D. Aliotta, M. Ananna, C. Barbieri, L. Barile, F. Bemmerer, D. Best, A. Broggini, C. Bruno, C. G. Caciolli, A. Campostrini, M. Casaburo, F. Cavanna, F. Colombetti, P. Compagnucci, A. Corvisiero, P. Csedreki, L. Davinson, T. De Gregorio, G. M. Dell'Aquila, D. Depalo, R. Di Leva, A. Elekes, Z. Ferraro, F. Formicola, A. Fülöp, Zs. Gervino, G. Guglielmetti, A. Gustavino, C. Gyürky, Gy. Imbriani, G. Junker, M. Lugaro, M. Marigo, P. Marsh, J. Masha, E. Menegazzo, R. Mercogliano, D. Paticchio, V. Perrino, R. Prati, P. Rigato, V. Robb, D. Schiavulli, L. Sidhu, R. S. Skowronski, J. Straniero, O. Szücs, T. Zavatarelli, S.
contents	The CNO cycle is one of the most important nuclear energy sources in stars. At temperatures of hydrostatic H-burning (20 MK $<$ T $<$ 80 MK) the $^{17}$O(p,$γ$)$^{18}$F reaction rate is dominated by the poorly constrained 64.5~keV resonance. Here we report on the first direct measurements of its resonance strength and of the direct capture contribution at 142 keV, performed with a new high sensitivity setup at LUNA. The present resonance strength of $ωγ_{(p, γ)}$\textsuperscript{bare} = (30 $\pm$ 6\textsubscript{stat} $\pm$ 2\textsubscript{syst})~peV is about a factor of 2 higher than the values in literature, leading to a $Γ$\textsubscript{p}\textsuperscript{bare} = (34 $\pm$ 7\textsubscript{stat} $\pm$ 3\textsubscript{syst})~neV, in agreement with LUNA result from the (p,$α$) channel. Such agreement strengthen our understanding of the oxygen isotopic ratios measured in red giant stars and in O-rich presolar grains.
format	Preprint
id	arxiv_https___arxiv_org_abs_2408_03015
institution	arXiv
publishDate	2024
record_format	arxiv
spellingShingle	First direct measurement of the 64.5 keV resonance strength in $^{17}$O(p,$γ$)$^{18}$F reaction Gesuè, R. M. Ciani, G. F. Piatti, D. Boeltzig, A. Rapagnani, D. Aliotta, M. Ananna, C. Barbieri, L. Barile, F. Bemmerer, D. Best, A. Broggini, C. Bruno, C. G. Caciolli, A. Campostrini, M. Casaburo, F. Cavanna, F. Colombetti, P. Compagnucci, A. Corvisiero, P. Csedreki, L. Davinson, T. De Gregorio, G. M. Dell'Aquila, D. Depalo, R. Di Leva, A. Elekes, Z. Ferraro, F. Formicola, A. Fülöp, Zs. Gervino, G. Guglielmetti, A. Gustavino, C. Gyürky, Gy. Imbriani, G. Junker, M. Lugaro, M. Marigo, P. Marsh, J. Masha, E. Menegazzo, R. Mercogliano, D. Paticchio, V. Perrino, R. Prati, P. Rigato, V. Robb, D. Schiavulli, L. Sidhu, R. S. Skowronski, J. Straniero, O. Szücs, T. Zavatarelli, S. Nuclear Experiment The CNO cycle is one of the most important nuclear energy sources in stars. At temperatures of hydrostatic H-burning (20 MK $<$ T $<$ 80 MK) the $^{17}$O(p,$γ$)$^{18}$F reaction rate is dominated by the poorly constrained 64.5~keV resonance. Here we report on the first direct measurements of its resonance strength and of the direct capture contribution at 142 keV, performed with a new high sensitivity setup at LUNA. The present resonance strength of $ωγ_{(p, γ)}$\textsuperscript{bare} = (30 $\pm$ 6\textsubscript{stat} $\pm$ 2\textsubscript{syst})~peV is about a factor of 2 higher than the values in literature, leading to a $Γ$\textsubscript{p}\textsuperscript{bare} = (34 $\pm$ 7\textsubscript{stat} $\pm$ 3\textsubscript{syst})~neV, in agreement with LUNA result from the (p,$α$) channel. Such agreement strengthen our understanding of the oxygen isotopic ratios measured in red giant stars and in O-rich presolar grains.
title	First direct measurement of the 64.5 keV resonance strength in $^{17}$O(p,$γ$)$^{18}$F reaction
topic	Nuclear Experiment
url	https://arxiv.org/abs/2408.03015