First measurement of the low-energy direct capture in <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mmultiscripts><mml:mi>Ne</mml:mi><mml:mprescripts/><mml:none/><mml:mn>20</mml:mn></mml:mmultiscripts><mml:mo>(</mml:mo><mml:mi>p</mml:mi><mml:mo>,</mml:mo><mml:mi>γ</mml:mi><mml:mo>)</mml:mo><mml:mmultiscripts><mml:mi>Na</mml:mi><mml:mprescripts/><mml:none/><mml:mn>21</mml:mn></mml:mmultiscripts></mml:mrow></mml:math> and improved energy and strength of the <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:msub><mml:mi>E</mml:mi><mml:mtext>c.m.</mml:mtext></mml:msub><mml:mo>=</mml:mo><mml:mn>368</mml:mn><mml:mspace width="0.16em"/><mml:mi>keV</mml:mi></mml:mrow></mml:math> resonance
E. Masha, L. Barbieri, J. Skowronski, M. Aliotta, C. Ananna, F. Barile, D. Bemmerer, A. Best, A. Boeltzig, C. Broggini, C. G. Bruno, A. Caciolli, M. Campostrini, Fausto Casaburo, F. Cavanna, G. F. Ciani, Agustín Ciapponi, P. Colombetti, Alessandro Compagnucci, P. Corvisiero, L. Csedreki, T. Davinson, R. Depalo, A. Di Leva, Z. Elekes, F. Ferraro, E. M. Fiore, A. Formicola, Zs. Fülöp, G. Gervino, A. Guglielmetti, C. Gustavino, Gy. Gyürky, G. Imbriani, J. José, M. Junker, Maria Lugaro, Pretima Manoj, Paola Marigo, R. Menegazzo, V. Paticchio, D. Piatti, P. Prati, D. Rapagnani, V. Rigato, D. Robb, L. Schiavulli, R. S. Sidhu, O. Straniero, T. Szücs, S. Zavatarelli
Abstract
The $^{20}\mathrm{Ne}{(p,\ensuremath{\gamma})}^{21}\mathrm{Na}$ reaction is the slowest in the NeNa cycle and directly affects the abundances of the Ne and Na isotopes in a variety of astrophysical sites. Here we report the measurement of its direct capture contribution, for the first time below ${E}_{\mathrm{c}.\mathrm{m}.}=352$ keV, and of the contribution from the ${E}_{\mathrm{c}.\mathrm{m}.}=368$ keV resonance, which dominates the reaction rate at $T=0.03$--1.00 GK. The experiment was performed deep underground at the Laboratory for Underground Nuclear Astrophysics, using a high-intensity proton beam and a windowless neon gas target. Prompt $\ensuremath{\gamma}$ rays from the reaction were detected with two high-purity germanium detectors. We obtain a resonance strength $\ensuremath{\omega}\ensuremath{\gamma}=(0.112\ifmmode\pm\else\textpm\fi{}0.{002}_{\mathrm{stat}}\ifmmode\pm\else\textpm\fi{}0.{005}_{\mathrm{sys}})\phantom{\rule{0.16em}{0ex}}\mathrm{meV}$, with an uncertainty a factor of 3 smaller than previous values. Our revised reaction rate is 20% lower than previously adopted at $T<0.1$ GK and agrees with previous estimates at temperatures $T\ensuremath{\ge}0.1$ GK. Initial astrophysical implications are presented.