Speaker
Dr
Marcell Peter Takacs
(Physikalisch-Technische Bundesanstalt)
Description
Among the solar fusion reactions, the rate of the $^7$Be($p,\gamma$)$^8$B reaction is one of the most difficult to determine. In a number of previous experiments, its astrophysical $S$-factor has been measured at $E$ = 0.1-2.5 MeV center-of-mass energy. However, no experimental data are available below 0.1 MeV. Thus, an extrapolation to solar energies is necessary, resulting in significant uncertainty for the extrapolated $S$-factor.
On the other hand, the flux of solar neutrinos has been recently measured with high precision, which provides an opportunity to turn the problem of the $S$-factor determination around: Using the measured $^7$Be and $^8$B neutrino fluxes, and the Standard Solar Model, the $^7$Be($p,\gamma$)$^8$B astrophysical $S$-factor is determined here at the solar Gamow peak.
Primary author
Dr
Marcell Peter Takacs
(Physikalisch-Technische Bundesanstalt)
Co-authors
Dr
Arnd Junghans
(HZDR)
Dr
Daniel Bemmerer
(HZDR)
Prof.
Kai Zuber
(TU Dresden)
