T. D. Shoppa

Solar fusion cross-sections

We review and analyze the available information on the nuclear-fusion cross sections that are most important for solar energy generation and solar neutrino production. We provide best values for the low-energy cross-section factors and, wherever possible, estimates of the uncertainties. We also describe the most important experiments and calculations that are required in order to improve our knowledge of solar fusion rates.

Information about the 12C(α,γ)16O reaction from the β-delayed proton decay of 17Ne

We are studying the β-delayed proton decay of 17Ne with the goal of determining the E2 part of the 12C(α,γ)16O cross section at energies relevant to helium burning in stars. We have determined branching ratios for proton and α-decay for states in 17F from 8.08 to 11.193 MeV. In addition, we have observed the break-up of the isobaric analogue state (IAS) at 11.193 MeV into three particles via two channels: proton decay to the 9.59 MeV state in 16O which breaks up into an α-particle plus 12C; and α-decay to the 2.365 MeV state in 13N which breaks up into a proton plus 12C. This is the first reported observation of the decay of the IAS to the 1− state in 16O at 9.59 MeV.

Extrapolation of the astrophysicalSfactor for7Be(p,γ)8Bto solar energies

We investigate the energy dependence of the astrophysical

Extrapolation of the astrophysical S factor for 7Be(p,γ)8B to solar energies

S

Has a standard model solution to the solar neutrino problem been found

factor for the reaction

Effect of the source charge on charged-boson interferometry

^7

Extrapolation of Astrophysical S Factors to Zero Energy

Be

{sup 7}Be({ital p},{gamma}){sup 8}B cross section and the properties of {sup 7}Be

(p,\gamma)^8

Three-particle breakup of the isobaric analog state in F-17

B, the primary source of high-energy solar neutrinos in the solar

Information about the C(,)O reaction from the -delayed proton decay of Ne

pp