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

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

1996-02-17

arxiv.org/abs/nucl-th/9602029v1

Phys.Rev.C53:2496-2504,1996

Physics

Nuclear Physics

Nuclear Theory

27 pages, 5 Postscript figures, uses RevTex and aps.sty; preprint also available at http://quasar.physik.unibas.ch/ Phys. Rev.

Scientific paper

10.1103/PhysRevC.53.2496

The reactions $^{10}$B(p,$\alpha$)$^{7}$Be and $^{11}$B(p,$\alpha$)$^{8}$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,$\alpha$)$^{7}$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,$\alpha_1$)$^{7}$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,$\alpha$)$^{8}$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.

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