dorsal/arxiv
View SchemaAstrophysical Reaction Rates for $^{10}$B(p,$\alpha$)$^{7}$Be and $^{11}$B(p,$\alpha$)$^{8}$Be From a Direct Model
| Authors | T. Rauscher, G. Raimann |
|---|---|
| Categories | |
| ArXiv ID | nucl-th/9602029 |
| URL | https://arxiv.org/abs/nucl-th/9602029 |
| DOI | 10.1103/PhysRevC.53.2496 |
| Journal | Phys.Rev.C53:2496-2504,1996 |
Abstract
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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"abstract": "The reactions $^{10}$B(p,$\\alpha$)$^{7}$Be and $^{11}$B(p,$\\alpha$)$^{8}$Be\nare studied at thermonuclear energies using DWBA calculations. For both\nreactions, transitions to the ground states and first excited states are\ninvestigated. In the case of $^{10}$B(p,$\\alpha$)$^{7}$Be, a resonance at\n$E_{Res}=10$ keV can be consistently described in the potential model, thereby\nallowing the extension of the astrophysical $S$-factor data to very low\nenergies. Strong interference with a resonance at about $E_{Res}=550$ keV\nrequire a Breit-Wigner description of that resonance and the introduction of an\ninterference term for the reaction $^{10}$B(p,$\\alpha_1$)$^{7}$Be$^*$. Two\nisospin $T=1$ resonances (at $E_{Res1}=149$ keV and $E_{Res2}=619$ keV)\nobserved in the $^{11}$B+p reactions necessitate Breit-Wigner resonance and\ninterference terms to fit the data of the $^{11}$B(p,$\\alpha$)$^{8}$Be\nreaction. $S$-factors and thermonuclear reaction rates are given for each\nreaction. The present calculation is the first consistent parametrization for\nthe transition to the ground states and first excited states at low energies.",
"arxiv_id": "nucl-th/9602029",
"authors": [
"T. Rauscher",
"G. Raimann"
],
"categories": [
"nucl-th",
"astro-ph"
],
"doi": "10.1103/PhysRevC.53.2496",
"journal_ref": "Phys.Rev.C53:2496-2504,1996",
"title": "Astrophysical Reaction Rates for $^{10}$B(p,$\\alpha$)$^{7}$Be and $^{11}$B(p,$\\alpha$)$^{8}$Be From a Direct Model",
"url": "https://arxiv.org/abs/nucl-th/9602029"
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