2006
DOI: 10.1140/epja/i2006-08-037-2
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Breakup of loosely bound nuclei as indirect method in nuclear astrophysics: 8B, 9C, 23Al

Abstract: Abstract. We discuss the use of one-nucleon breakup reactions of loosely bound nuclei at intermediate energies as an indirect method in nuclear astrophysics. These are peripheral processes, therefore we can extract asymptotic normalization coefficients (ANC) from which reaction rates of astrophysical interest can be inferred. To show the usefulness of the method, three different cases are discussed. In the first, existing experimental data for the breakup of 8 B at energies from 30 to 1000 MeV/u and of 9 C at … Show more

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Cited by 3 publications
(22 citation statements)
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“…Indeed, assuming such an inversion, we recalculate the astrophysical S factor (Fig. 1) and the stellar reaction rate for the 22 Mg(p,γ ) 23 Al reaction and find an increase of 30 to 50 times over the current estimate of the rate for the temperature range of ONe novae; viz.,T 9 = 0.1-0.5 (see also [22]). This is due to the larger proton penetration for an s-wave capture and the absence of a centrifugal barrier for the last proton in 23 Al, which allows the wave function of the barely bound proton in the final state to extend far beyond the nuclear interior, thus increasing its overlap with the wave function of the incoming proton.…”
Section: Astrophysical Motivationmentioning
confidence: 95%
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“…Indeed, assuming such an inversion, we recalculate the astrophysical S factor (Fig. 1) and the stellar reaction rate for the 22 Mg(p,γ ) 23 Al reaction and find an increase of 30 to 50 times over the current estimate of the rate for the temperature range of ONe novae; viz.,T 9 = 0.1-0.5 (see also [22]). This is due to the larger proton penetration for an s-wave capture and the absence of a centrifugal barrier for the last proton in 23 Al, which allows the wave function of the barely bound proton in the final state to extend far beyond the nuclear interior, thus increasing its overlap with the wave function of the incoming proton.…”
Section: Astrophysical Motivationmentioning
confidence: 95%
“…γ rays from the decay of longlived isotopes like 26 Al (t 1/2 = 7.2 × 10 5 yr), 44 Ti (60.0 yr), 56 Ni (6.1 d), etc., have been detected. Among the expected γ -ray emitters is 22 Na (t 1/2 = 2.6 yr), thought to be produced in the thermonuclear runaway and in the high-temperature phase of so-called ONe novae (oxygen-neon novae) through the reaction chain 20 Ne(p,γ ) 21 Na(p,γ ) 22 Mg(βγ ) 22 Na-the NeNa cycle [1][2][3][4]. Measurements, however, have not detected the 1.275 MeV γ ray that follows the decay of 22 Na and have only been able to set an upper limit on its production, a limit which is below the theoretical predictions (see, for example, [5,6] and the references therein).…”
Section: Introductionmentioning
confidence: 99%
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