= Solar neutrino detection
<Solar neutrino detection> asks how an invisible <electron neutrino> from the <Sun> becomes a measurable laboratory record. The <Homestake experiment> stores a reaction product for later counting; <Kamiokande> records light promptly. The former measures an exposure-integrated rate, whereas the latter can retain event times and statistical source-direction information. These are complementary ways to connect <stellar nuclear fusion> with <neutrino astronomy>.
A detector samples a weighted part of a <neutrino flux>, rather than counting every passing <neutrino>. For a target population $N_T$, an ideal reaction rate is
$$
R=N_T\int_{E_{\min}}^\infty\phi_e(E)\sigma_e(E)\,dE,
$$
where $\phi_e(E)$ is the differential <electron neutrino> <neutrino flux> and $\sigma_e(E)$ is the relevant <cross section>. A <detection efficiency> belongs inside the <integral> if it depends on <energy>. Two detectors can therefore disagree in raw count rate while observing the same source. Interpreting a deficit requires both a source prediction and a detector response.
Back to article page
