Solar neutrino cross sections.
Numerical values for different solar neutrino cross sections are available
at this url.
Solar Neutrino Cross Sections and Nuclear
Author(s): John Bahcall
Journal: Physical Review, 135, B137 (July 1964).
The neutrino-producing reactions that are believed to occur in the
interior of the sun are reviewed and the predicted neutrino fluxes
from these reactions are presented. The relevant absorption cross
sections for neutrino-induced transitions from the ground state of
Cl37 to various states in Ar37 are then
calculated. The nuclear model adopted in these calculations is also
used to predict the decay rates and branching ratios for a number of
nuclei with 1d3/2n configurations;
comparisons with experiment are made wherever possible and additional
tests are suggested. A method for extracting Gamow-Teller matrix
elements from mixed transitions between members of the same isotopic
multiplet is then illustrated. The theory of bound-state neutrino
capture is also outlined and applied to the proposed solar neutrino
experiment. In an Appendix, some neutrino cross sections that are
useful in interpreting the reactor experiment of Davis are presented.
neutrino experiments: absorption cross sections, neutrino spectra, and
predicted event rates
Author(s): John Bahcall
Journal: Phys. Rev. C, 56, No. 6,
3391-3409 (December 1997),
Neutrino absorption cross sections for 71Ga
are calculated for all solar neutrino sources
with standard energy spectra, and for laboratory sources of 51Cr
the calculations include, where appropriate,
the thermal energy of decaying
solar ions and
use improved nuclear and atomic data.
The ratio, R, of measured (in GALLEX
and SAGE) to calculated 51Cr capture rate
is R = 0.95 ± 0.07 (exp) +0.04-0.03 (theory).
Cross sections are also calculated for specific
neutrino energies chosen so that a spline fit
the event rates in a gallium detector even if new physics
changes the energy spectrum of solar neutrinos. Theoretical
uncertainties are estimated for cross sections at specific energies
and for standard neutrino energy spectra.
energy spectra are presented for pp and CNO neutrino
sources in the appendices.
Neutrino fluxes predicted by standard solar models,
diffusion, have been in the
range 120 SNU to 141 SNU since 1968.
Solar neutrinos: radiative corrections in neutrino-electron scattering experiments
Author(s): John N. Bahcall, Marc Kamionkowski, and Alberto Sirlin
Journal: Physical Review D, 51, 6146-6158
(June 1, 1995); astro-ph/9502003.
Abstract: Radiative corrections to the
electron recoil energy spectra and to total cross sections are
for neutrino-electron scattering by solar neutrinos. Radiative
corrections change monotonically the electron recoil spectrum for
neutrinos, with the relative probability of observed recoil electrons
being reduced by about 4 percent at the highest electron energies.
For p-p and berylium neutrinos, the recoil spectra are not affected
significantly. Total cross sections for solar neutrino-electron
scattering are reduced by about 2 percent compared to previously
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