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L.M. Malyshkin, R.M. Kulsrud (Princeton University Observatory)
We consider the possibility of MSW time variations of the
solar neutrino flux due to neutrino interference effects.
For two types of neutrinos there are two MSW neutrino
solutions, + and -. In vacuum these are the m1 and
m2 (m1 Two necessary criteria to observe neutrino flux time
variations are proposed. The first criterion,
\sigma{{\lower.5ex\;\buildrel{\mbox{\footnotesize<}}\over{\mbox{\footnotesize\sim}}\;}}\sigmat,
for the time variation not to be averaged to zero over the
detection energy width \sigma, should be satisfied. In the
case of the 0.862\,{\rm Mev} 7Be solar neutrino line
this criterion gives us an upper estimate for m22-m12,
the difference of neutrino mass squared, of ~
10-9{\rm ev}2. The second criterion,
\sigmaa{{\lower.5ex\;\buildrel{\mbox{\footnotesize<}}\over{\mbox{\footnotesize\sim}}\;}}\sigmat,
is necessary for collisional coherence to exist. This
criterion is equivalent to a plausible condition
a|t+2-t-2|{{\lower.5ex\;\buildrel{\mbox{\footnotesize<}}\over{\mbox{\footnotesize\sim}}\;}}
{{\!\,\lambda\!\!\!\!\!\stackrel{-}{\phantom{__}}\!\,}}.
Our criterion is stronger than collisional coherence
criteria formerly suggested, which are roughly equivalent to
the condition
a|t+2-t-2|{{\lower.5ex\;\buildrel{\mbox{\footnotesize<}}\over{\mbox{\footnotesize\sim}}\;}}
l, because the neutrino De Broglie wavelength
{{\!\,\lambda\!\!\!\!\!\stackrel{-}{\phantom{__}}\!\,}}
is much less than the interparticle distance in the solar
interior l.
Exact values for the detected neutrino flux and its
variations will be presented for both the case of a solar
neutrino line, and the case of a continuous neutrino
spectrum with a Gaussian shape of the energy response
function of the neutrino detection device.
The author(s) of this abstract have provided an email address
for comments about the abstract:
leonmal@astro.princeton.edu