Neutrino counting

We thus see that the non-minimal model in lowest order gives precisely the results of the higher order corrections to the minimal model with g — go- Thus, once again (see Section 7.9) the interpertation of a measurement that finds 1 is not absolutely straightforward. 

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We focus on four major topics (i) the angular distributions (ii) determination of the parameters of the Z (iii) neutrino counting and (iv) asymmetries and polarisation measurements. The major source of information comes from the reactions ... 

For some experiments, the solar neutrino flux and the rate of decay of the proton being extreme examples, tire count rate is so small that observation times of months or even years are required to yield rates of sufficiently small relative uncertainty to be significant. For high count rate experiments, the limitation is the speed with which the electronics can process and record the incoming infomiation. 

The Total Leplon Number Remains Constant. Leptons consist of the neutrinos, electrons, muons, and their antipanieles Here again, rhe basic principles applied are analogous to those for baryon number particles count 1 antipanieles count - I and baryons and mesons 0. 

Some years later, a Japanese-built detector (Kamiokaride II), designed to delect the more energetic solar-emitted neutrinos ( -5 mil electron volts), came up about 50% short of the expected counts, thus reconfirming a shortage of solar neutrons. 

One of the areas in which the skills of radiochemists are used is the area of low-level chemistry and low-level counting. Areas as diverse as the detection of solar neutrinos or the study of environmental radioactivity involve low-level techniques. For example, despite concentration of the radiotracers of interest during sampling procedures in environmental studies, quite often one is left with a sample containing... 

Neutrinos no longer count as "dark matter candidates" since they are known experimentally to oscillate among flavors and so to have non-zero rest masses. The implied masses are such that the ones we know and love contribute less than Qv = 0.01 (ApOO, Sect. 12.4.2). Observed large scale structure and models for its formation are happiest with Qv = 0.006 or thereabouts. (57)... 

Search for Supernovae. The copious flux of neutrinos originating from a SN produces low energy positrons that emit Cherenkov light throughout the detector. Coincidently with a SN explosion, the collective count rates summed... 

UHECRs are attractive because of their high centre-of mass energy. The proton-nucleon cross section for BH formation is very small compared to other hadronic processes. The neutrino-nucleon cross section for BH formation may be higher than the SM process, thereby giving interest to neutrino interaction. However, rate counting is not sufficient to prove black hole formation in the atmosphere. Discovery of BHs in UHECRs requires discrimination of BH and SM air showers. The extensive air shower (EAS) characteristics of these processes will differ, and with new detector methods and enough statistics expected from the new generation cosmic ray observatories, it may be possible to detect BH-induced EASs. 

A large international collaboration ("Gallex ) is setting up a neutrino detection station in a rock facility in the Mont Blanc. Some Ga atoms in 30 tons of gallium metal is expected to react with solar neutrinos to form Ge (t, 11.4 d) which is to be converted to the gaseous hydride, GeH, and counted in a proportional detector. About 1 atom of Ge formed per day is expected. 

Elementary particles come in only two kinds quarks and leptons. There are only six quarks and six leptons, see Table 10.2. The leptons are the electron, e, the muon, fi, and the tauon (tau particle), t, and their respective neutrinos. The quarks and leptons are grouped together in three families (or generations) of two quarks and two leptons each. This makes 12 elementary building blocks, or 24 if one counts their anti particles Table 10.2 only refers to our matter (i.e. koino matter). The leptons and quarks all have different properties and names, sometimes also referred to as colors. The physical theory relating these particles to each other is therefore named Quantum Chromo Dynamics (QCD). 

It is felt that a real neutrino mass as large as 10-15 eV would cause observable spectral distortions even in the presence of the end-point count excesses. 

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