Astrophysical Reaction Rates for $^{10}$B(p,$α$)$^{7}$Be and $^{11}$B(p,$α$)$^{8}$Be From a Direct Model

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dc.creatorRauscher, T.
dc.creatorRaimann, G.
dc.date1996-02-17
dc.date.accessioned2026-07-07T11:15:39Z
dc.date.available2026-07-07T11:15:39Z
dc.descriptionThe reactions $^{10}$B(p,$α$)$^{7}$Be and $^{11}$B(p,$α$)$^{8}$Be are studied at thermonuclear energies using DWBA calculations. For both reactions, transitions to the ground states and first excited states are investigated. In the case of $^{10}$B(p,$α$)$^{7}$Be, a resonance at $E_{Res}=10$ keV can be consistently described in the potential model, thereby allowing the extension of the astrophysical $S$-factor data to very low energies. Strong interference with a resonance at about $E_{Res}=550$ keV require a Breit-Wigner description of that resonance and the introduction of an interference term for the reaction $^{10}$B(p,$α_1$)$^{7}$Be$^*$. Two isospin $T=1$ resonances (at $E_{Res1}=149$ keV and $E_{Res2}=619$ keV) observed in the $^{11}$B+p reactions necessitate Breit-Wigner resonance and interference terms to fit the data of the $^{11}$B(p,$α$)$^{8}$Be reaction. $S$-factors and thermonuclear reaction rates are given for each reaction. The present calculation is the first consistent parametrization for the transition to the ground states and first excited states at low energies.
dc.description27 pages, 5 Postscript figures, uses RevTex and aps.sty; preprint also available at http://quasar.physik.unibas.ch/ Phys. Rev. C, in press
dc.identifierhttps://arxiv.org/abs/nucl-th/9602029
dc.identifierhttp://arxiv.org/abs/nucl-th/9602029
dc.identifierPhys.Rev.C53:2496-2504,1996
dc.identifierdoi:10.1103/PhysRevC.53.2496
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/192456
dc.subjectNuclear Theory
dc.subjectAstrophysics
dc.titleAstrophysical Reaction Rates for $^{10}$B(p,$α$)$^{7}$Be and $^{11}$B(p,$α$)$^{8}$Be From a Direct Model
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