New constraints on the <math xmlns="http://www.w3.org/1998/Math/MathML"><mrow><mmultiscripts><mi>Al</mi><mprescripts></mprescripts><none></none><mn>25</mn></mmultiscripts><mo>(</mo><mi>p</mi><mo>,</mo><mi>γ</mi><mo>)</mo></mrow></math> reaction and its influence on the flux of cosmic <math xmlns="http://www.w3.org/1998/Math/MathML"><mi>γ</mi></math> rays from classical nova explosions

L. Canete; G. Lotay; G. Christian; D. T. Doherty; W. N. Catford; S. Hallam; D. Seweryniak; H. M. Albers; S. Almaraz-Calderon; E. A. Bennett; M. P. Carpenter; C. J. Chiara; J. P. Greene; C. R. Hoffman; R. V. F. Janssens; J. José; A. Kankainen; T. Lauritsen; A. Matta; M. Moukaddam; S. Ota; A. Saastamoinen; R. Wilkinson; S. Zhu

doi:10.1103/PhysRevC.104.L022802

Letter

New constraints on the ${}^{25}{Al} (p, γ)$ reaction and its influence on the flux of cosmic $γ$ rays from classical nova explosions

L. Canete ¹, G. Lotay¹, G. Christian^2,3,4,*, D. T. Doherty¹, W. N. Catford¹, S. Hallam¹, D. Seweryniak⁵, H. M. Albers^5,†, S. Almaraz-Calderon^5,‡ et al.

E. A. Bennett ^2,6, M. P. Carpenter⁵, C. J. Chiara^5,7,§, J. P. Greene ⁵, C. R. Hoffman⁵, R. V. F. Janssens ^8,9, J. José ^10,11, A. Kankainen ^12,13, T. Lauritsen ⁵, A. Matta ^1,∥, M. Moukaddam^1,¶, S. Ota ², A. Saastamoinen², R. Wilkinson¹, and S. Zhu^5,#

¹Department of Physics, University of Surrey, Guildford GU2 7XH, United Kingdom
²Cyclotron Institute, Texas A&M University, College Station, Texas 77843, USA
³Department of Physics and Astronomy, Texas A&M University, College Station, Texas 77843, USA
⁴Nuclear Solutions Institute, Texas A&M University, College Station, Texas 77843, USA
⁵Physics Division, Argonne National Laboratory, Argonne, Illinois 60439, USA
⁶Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USA
⁷Department of Chemistry and Biochemistry, University of Maryland, College Park, Maryland 20742, USA
⁸Department of Physics, University of North Carolina at Chapel Hill, Chapel Hill, North Carolina 27599, USA
⁹Triangle Universities Nuclear Laboratory, Duke University, Durham, North Carolina 27708, USA
¹⁰Departament de Física, Universitat Politècnica de Catalunya, E-08019 Barcelona, Spain
¹¹Institut d'Estudis Espacials de Catalunya (IEEC), E-08034 Barcelona, Spain
¹²School of Physics and Astronomy, University of Edinburgh, Edinburgh EH9 3JZ, United Kingdom
¹³Department of Physics, University of Jyväskylä, FI-40014 Jyväskylä, Finland

^*Present address: Department of Astronomy and Physics, Saint Mary's University, Halifax, Nova Scotia B3H 3C3, Canada.
^†Present address: GSI Helmholtzzentrum für Schwerionenforschung GmbH, 64291 Darmstadt, Germany.
^‡Present address: Department of Physics, Florida State University, Tallahassee, Florida 32306, USA.
^§Present address: U.S. Army Research Laboratory, Adelphi, Maryland 20783, USA.
^∥Present address: Laboratoire de Physique Corpusculaire de Caen, 14050 CAEN CEDEX 4, France.
^¶Present address: Université de Strasbourg, IPHC, 23 Rue du Loess, 67037 Strasbourg, France.
^#Present address: National Nuclear Data Center, Brookhaven National Laboratory, Upton, New York 11973, USA.

PDF

Phys. Rev. C 104, L022802 – Published 16 August, 2021

DOI: https://doi.org/10.1103/PhysRevC.104.L022802

Abstract

The astrophysical ${}^{25}{Al} (p, γ) {}^{26}{Si}$ reaction represents one of the key remaining uncertainties in accurately modeling the abundance of radiogenic ${}^{26}{Al}$ ejected from classical novae. Specifically, the strengths of key proton-unbound resonances in ${}^{26}{Si}$ , that govern the rate of the ${}^{25}{Al} (p, γ)$ reaction under explosive astrophysical conditions, remain unsettled. Here, we present a detailed spectroscopy study of the ${}^{26}{Si}$ mirror nucleus ${}^{26}{Mg}$ . We have measured the lifetime of the $3^{+}$ , 6.125-MeV state in ${}^{26}{Mg}$ to be $19 (3) fs$ and provide compelling evidence for the existence of a $1^{-}$ state in the $T = 1, A = 26$ system, indicating a previously unaccounted for $ℓ = 1$ resonance in the ${}^{25}{Al} (p, γ)$ reaction. Using the presently measured lifetime, together with the assumption that the likely $1^{-}$ state corresponds to a resonance in the ${}^{25}{Al} + p$ system at 435.7(53) keV, we find considerable differences in the ${}^{25}{Al} (p, γ)$ reaction rate compared to previous works. Based on current nova models, we estimate that classical novae may be responsible for up to $\approx 15 %$ of the observed galactic abundance of ${}^{26}{Al}$ .

Physics Subject Headings (PhySH)

Authorization Required

We need you to provide your credentials before accessing this content.

Article Available via CHORUS

Download Accepted Manuscript

Physical Review C

Export citation

Export citation

New constraints on the ${}^{25}{Al} (p, γ)$ reaction and its influence on the flux of cosmic $γ$ rays from classical nova explosions

Abstract

Physics Subject Headings (PhySH)

Authorization Required

Other Options

References (Subscription Required)

Outline

Information

Filter

Filter

Article Lookup

Enter a citation

New constraints on the Al25(p,γ) reaction and its influence on the flux of cosmic γ rays from classical nova explosions

Abstract

Physics Subject Headings (PhySH)

Authorization Required

Log in via your institution

Log in via APS Member Subscription

Other Options

References (Subscription Required)

New constraints on the ${}^{25}{Al} (p, γ)$ reaction and its influence on the flux of cosmic $γ$ rays from classical nova explosions