1. Gamma width ofO*14(5.17 MeV) and the stellarN13(p,γ)14O reaction rate
- Author
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Stephen Sanders, Michael Scott Smith, Eric Adelberger, P. B. Fernandez, T. F. Wang, P. V. Magnus, Alejandro L. Garcia, Curley Rm, K. I. Hahn, P. D. Parker, and K. E. Rehm
- Subjects
Reaction rate ,Nuclear reaction ,Physics ,Nuclear and High Energy Physics ,Light nucleus ,CNO cycle ,Branching fraction ,Excited state ,Radiative capture ,Analytical chemistry ,Atomic physics - Abstract
We have determined the [gamma]-ray branching ratio [Gamma][sub [gamma]]/[Gamma][sub tot] for the first excited state in [sup 14]O ([ital E][sub [ital x]]=5.17 MeV) to be (3.1[plus minus]1.7)[times]10[sup [minus]4], corresponding to a [gamma] width of 12[plus minus]7 eV. This value was determined by measuring the ratio of the [sup 14]N([ital p],[ital n])[sup 14]O[sub 0] to [sup 14]N([ital p],[ital n])[sup 14]O[sub 1] cross sections via neutron time of flight, and the ratio of [sup 14]N([ital p],[ital n])[sup 14]O[sub 0] to [sup 14]N([ital p],[ital n])[sup 14]O[sub 1]([gamma])[sup 14]O[sub 0] cross sections at the same center-of-mass energy by bombarding a hydrogen target with a [sup 14]N beam and kinematically distinguishing the [sup 14]O[sub 0] recoils from the two reaction channels. The present value for [Gamma][sub [gamma]] is consistent with other measurements at the 2-[sigma] level; a weighted mean of all measurements is used to calculate the stellar [sup 13]N([ital p],[gamma])[sup 14]O reaction rate, and thereby determine the temperatures and densities at which the stellar carbon-nitrogen-oxygen (CNO) cycle is converted to the hot CNO cycle.
- Published
- 1993
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