Abstract
We use a configuration-mixing quasiparticle Tamm-Dancoff approximation to calculate the expected event rate for an $^{127}\mathrm{I}$ solar neutrino detector. Our cross section for $^{8}\mathrm{B}$ solar neutrinos is 2.2\ifmmode\times\else\texttimes\fi{}${10}^{\mathrm{\ensuremath{-}}42}$ ${\mathrm{cm}}^{2}$ [corresponding to about 13 solar neutrino units (SNU) in the standard solar model], a factor of more than 3 below an estimate by Haxton. This value may increase by about 30% when quadrupole correlations are included. The cross section for ``Be neutrinos is 2.0\ifmmode\times\else\texttimes\fi{}${10}^{\mathrm{\ensuremath{-}}45}$ ${\mathrm{cm}}^{2}$ (9.4 SNU), in agreement with a calculation by Dellagiacoma and Iachello. The total event rate per nucleus from all solar neutrinos is about 3 times that in $^{37}\mathrm{Cl}$.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
