Radiative capture reaction<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mo>(</mml:mo><mml:mi mathvariant="normal">p</mml:mi></mml:mrow><mml:mprescripts/><mml:mrow/><mml:mrow><mml:mn>7</mml:mn></mml:mrow><mml:mrow/><mml:mrow/></mml:mmultiscripts></mml:mrow></mml:math>,γ<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msup><mml:mrow><mml:mo>)</mml:mo></mml:mrow><mml:mrow><mml:mn>8</mml:mn></mml:mrow></mml:msup></mml:mrow></mml:math>B at low energies
K. H. KimDepartment of Physics, Sung Kyun Kwan University, Suwon, 170, KoreaMoon Ho ParkDepartment of Physics, Sung Kyun Kwan University, Suwon, 170, KoreaB. T. KimDepartment of Physics, Sung Kyun Kwan University, Suwon, 170, Korea
1987lv
ABI
Abstract
We calculated the differential cross sections as well as the total cross sections for the $^{7}\mathrm{Be}$(p,\ensuremath{\gamma}${)}^{8}$B at low energies in the radiative direct capture model including the E1, M1, and E2 transitions. The astrophysical S factor at the solar temperature of 20 keV is found to be 0.024 keV? which agrees well with a recent measurement by Filippone et al. We show that the d-wave capture plays an important role in determining the magnitude and shape of S(E) at low energies of astrophysical interest.
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