  The standard solar model (SSM) yield a $^8$B solar neutrino flux which is
consistent within the theoretical and experimental uncertainties with that
observed at Super-Kamiokande. The combined results from the Super- Kamiokande
and the Chlorine solar neutrino experiments do not provide a solid evidence for
neutrino properties beyond the minimal standard electroweak model. The results
from the Gallium experiments and independently the combined results from
Super-Kamiokande and the Chlorine experiment imply that the $^7$Be solar
neutrino flux is strongly suppressed compared with that predicted by the SSM.
This conclusion, however, is valid only if the neutrino absorption cross
sections near threshold in Gallium and Chlorine do not differ significantly
from their theoretical estimates. Such a departure has not been ruled out by
the Chromium source experiments in Gallium. Even if the $^7$Be solar neutrino
flux is suppressed compared with that predicted by the SSM, still it can be due
to astrophysical effects not included in the simplistic SSM. Such effects
include spatial and/or temporal variations in the temperature in the solar core
induced by the convective layer through g-modes or by rotational mixing in the
solar core, and dense plasma effects which may strongly enhance p-capture by
$^7$Be relative to e-capture. The new generation of solar observations, which
already look non stop deep into the sun, like Super-Kamiokande through
neutrinos, and SOHO and GONG through acoustic waves, may be able to point at
the correct solution; astrophysical solutions if they detect unexpected
temporal and/or spatial behaviour, or particle physics solutions if
Super-Kamiokande detects characteristic spectral distortion or temporal
variations (e.g., the day-night effect) of the $^8$B solar neutrino flux . If
