Neutrino scattering

When we come to deal with neutrino scattering we shall have a current that is not conserved and the F3 type form factor will appear. The form factors Fi,F2 are defined in such a way that for q = 0, which physically corresponds to the proton interacting with a static electro-magnetic field, one has... 

The reader is warned that in some literature qs is defined a factor of 2 larger than ours is.) This estimate is supported by data on charm production in deep inelastic neutrino scattering where the dominant transition is s c (see Section 18.2). 

In conclusion, we mention the following statistically weak observational oddities the 7 sec time gap in Kamiokande data, the lack of late time events in IM8, the occurrence of two possible electron scattering events very early in time, and the discrepancy of the Kamiokande and IMB average neutrino energies. The work on particle models is being pursued with G. Fuller, R. Mayle, K. Olive, D. Schramm. 

The Sudbury Neutrino Observatory (SNO) detector, located at Sudbury, Ontario, Canada, consists of 1000 tons of heavy water (D20) mounted 2 km below the surface in the Sudbury Nickel Mine. In addition to neutrino-electron scattering, this detector can also utilize nuclear reactions involving deuterium ... 

J. P. Vigier, Charmed quark discovery in anti-neutrino nucleon scattering Lett. Nuovo Cimento 15(2) (Ser. 2), 41 48 (1976). 

Figure 16.17. Complementarity of direct and indirect neutralino dark matter searches. The figure shows that several supersymmetric models that are within the (expected) reach of a big neutrino telescope of 10 km2 yr exposure are beyond the reach of current and future direct detection experiments. The vertical axis is the product of the neutralino-proton spin-independent scattering cross section

Neutrino weak interaction cross section is dominated at E > 100 GeV by charged current Deep Inelastic Scattering (DIS) [33] ... 

Electron scattering by photons may alternatively result in pair neutrino production, with a nett energy loss as shown ... 

The synthesis of the light elements is sensitive to physical conditions in the early radiation-dominated era at temperatures T < 1 MeV, corresponding to an age r > 1 s. At these and higher temperatures, weak interactions rates Tweak > H were rapid compared to the expansion rate, and thus the weak interactions were in thermal equilibrium. In particular, the processes which interconvert neutrons and protons through scatterings with electrons (e ), positrons (e ), electron neutrinos (ve) and electron anti-neutrinos (v ), namely... 

In this reaction, the e is a positron and the Ve is an electron-type neutrino. Significantly, this reaction depends on the weak force since it requires one of the two reacting protons to convert into a neutron in the brief moment the two protons are in close contact. This is rare, so the vast majority of proton-proton scatterings in a star do not result in deuterium production. The deuterium, that is, the H, produced by the pp reaction quickly captures a proton to become He ... 

To repeat what was said above, there is no indication whatever that the cross section for the scattering of neutrinos by heavy particles is actually as high as the above figures are. On the other hand, there is at present no obvious experimental evidence which would show that the cross section is below the above figures. Fermi has pointed out to the writer that if the neutrinos created in the sun could freely escape, they would have a density comparable to the... 

Turning to the other process, the scattering cross section of neutrinos by electrons, for which Nahmias investigation was imdertaJcen, there is no reason to modify his and Bethe s conclusions (ibid, p. 108). The cross section in this case is less than 10 " cm. ... 

The neutrino flux of a core-collapse supernova is high enough to contribute to the nucleosynthesis of certain rare elements and isotopes, even in the outer layers of the star. In this so-called v-process, inelastic scattering of a neutrino leads to formation of an excited daughter nuclide, which then decays by particle emission. This process can contribute significantly to the production of light ( B, and heavy ( La, Ta) nuclides (Woosley and Weaver 1995 Heger et al. 2005). 

The predicted neutral current weak interaction was initially seen in neutrino-nucleon scattering in 1973. There remained the question of the validity of the theory as regards parity violation in the electron-nucleon interaction. This question has been largely answered in high-energy electronscattering experiments and in the atomic parity violation experiments, the subject of this review. 

---