Study of ^8Li and the astrophysical S_17(0) factor

Details Study of ^8Li and the astrophysical S_17(0) factor Study of ^8Li and the astrophysical S_17(0) factor

Oct 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aps..dnp.db003t&link_type=abstract

American Physical Society, Division of Nuclear Physics Meeting, October 4-7, 2000 Williamsburg, VA, abstract #DB.003

Physics

Nuclear Physics

Scientific paper

We showed before that one can determine the astrophysical factor S_17(0) for the proton radiative capture reaction ^7Be(p,γ)^8B from the precise determination of the tail of the wave function of the last proton in the g.s. of ^8B (Asymptotic Normalization Coefficient method) using transfer reactions [1]. It is likely that reliable information about the structure of ^8B could be obtained from the study of its mirror nucleus ^8Li. Therefore, in addition to our previously reported proton transfer reactions (^7Be,^8B) we investigated the mirror neutron transfer reaction ^13C(^7Li,^8Li)^12C for the study of ^8Li. The data allowed us to disentangle the relative contributions of the p_3/2 and p_1/2 orbitals to the ground state of ^8Li, which was not practical for ^8B due to the finite angular resolution in the radioactive beam study. We find C^2_p_1/2/C^2_p_3/2=0.13(2), in good agreement with the calculated ratio [2] we used in determining S_17(0) previously [1]. ^1A. Azhari et al., Phys. Rev. Lett 82, 3960 (1999); Phys. Rev. C60, 055803 (1999) and this meeting; ^2A. M. Mukhamedzhanov and N. K. Timofeyuk, Sov. J. Phys. 51, 431 (1990) This work was supported by DOE and the Robert A. Welch Foundation.

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