ABSTRACT
The expectations of what should be observed in solar neutrino experiments can be conveniently organized into four categories: A) Neutrino Cross Sections, B) Early Solar Models, C) Sensitivity Studies, and D) Refined Solar Models. The expectations discussed in this section depend upon both the standard electroweak model, which implies that essentially nothing happens to solar neutrinos from the time they are created in the center of the sun until they arrive at detectors on earth (but see Section IV), and the standard solar model, which can be used to predict the fluxes of neutrinos of different energies that are produced in the sun.
