Astrophysical rate of <span class="aps-inline-formula"><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msup><mrow></mrow><mrow><mn>15</mn></mrow></msup></mrow><mi mathvariant="normal">O</mi><mo>(</mo><mi>α</mi><mo>,</mo><mi>γ</mi><mrow><msup><mrow><mo>)</mo></mrow><mrow><mn>19</mn></mrow></msup></mrow><mi mathvariant="normal">Ne</mi></math></span> via the <span class="aps-inline-formula"><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mn></mn><mo>(</mo><mi>p</mi><mo>,</mo><mi>t</mi><mo>)</mo><mn></mn></math></span> reaction in inverse kinematics

B. Davids; A. M. van den Berg; P. Dendooven; F. Fleurot; M. Hunyadi; M. A. de Huu; R. H. Siemssen; H. W. Wilschut; H. J. Wörtche; M. Hernanz; J. José; K. E. Rehm; A. H. Wuosmaa; R. E. Segel

doi:10.1103/PhysRevC.67.065808

Astrophysical rate of $^{15} O (α あるふぁ, γ がんま)^{19} Ne$ via the $(p, t)$ reaction in inverse kinematics

B. Davids, A. M. van den Berg, P. Dendooven, F. Fleurot, M. Hunyadi, M. A. de Huu, R. H. Siemssen, H. W. Wilschut, H. J. Wörtche, M. Hernanz, J. José, K. E. Rehm, A. H. Wuosmaa, and R. E. Segel

Phys. Rev. C 67, 065808 – Published 27 June 2003

Abstract

A recoil coincidence technique has been applied to measure the $α あるふぁ$ -decay branching ratios of near-threshold states in $^{19} Ne .$ Populating these states using the $(p, t)$ reaction in inverse kinematics, we detected the recoils and their decay products with 100% geometric efficiency using a magnetic spectrometer. Combining our branching ratio measurements with independent determinations of the radiative widths of these states, we calculate the astrophysical rate of $^{15} O (α あるふぁ, γ がんま)^{19} Ne .$ Using this reaction rate, we perform hydrodynamic calculations of nova outbursts and conclude that no significant breakout from the hot CNO cycles into the $rp$ process occurs in novae via $^{15} O (α あるふぁ, γ がんま)^{19} Ne .$

Received 24 March 2003

DOI:https://doi.org/10.1103/PhysRevC.67.065808

Authors & Affiliations

B. Davids^*, A. M. van den Berg, P. Dendooven, F. Fleurot^†, M. Hunyadi, M. A. de Huu, R. H. Siemssen, H. W. Wilschut, and H. J. Wörtche

Kernfysisch Versneller Instituut, Zernikelaan 25, 9747 AA Groningen, The Netherlands

M. Hernanz

Institut d’Estudis Espacials de Catalunya, Ed. Nexus-201, C/Gran Capità 2-4, E-08034 Barcelona, Spain

J. José

Institut d’Estudis Espacials de Catalunya, Ed. Nexus-201, C/Gran Capità 2-4, E-08034 Barcelona, Spain
Departament de Física i Enginyeria Nuclear, Universitat Politècnica de Catalunya, Av. Victor Balaguer s/n E-08800 Vilanova i la Geltrú, Barcelona, Spain

K. E. Rehm and A. H. Wuosmaa^‡

Physics Division, Argonne National Laboratory, Argonne, Illinois 60439, USA

R. E. Segel

Department of Physics, Northwestern University, Evanston, Illinois 60208, USA

^*Email address: davids@kvi.nl
^†Present address: Department of Physics, Laurentian University, Sudbury, ON, Canada P3E 2C6.
^‡Present address: Department of Physics, Western Michigan University, Kalamazoo, MI 49008.

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Vol. 67, Iss. 6 — June 2003

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