|Statement||edited by Vernon Barger & David Cline.|
|Contributions||Barger, V. 1938-, Cline, D. 1933-|
|LC Classifications||QC793.5.N426 N49 1985|
|The Physical Object|
|Pagination||ix, 416 p. :|
|Number of Pages||416|
|LC Control Number||85029640|
4. Low energy neutrino interactions. Neutrino–hadron interactions have been observed over a wide energy range, from keV for solar neutrinos up to energies of several GeV in the case of accelerator : F. Vannucci. Solar neutrino studies can also contribute to our understanding of the nature of neutrino interactions. The electron-neutrino survival probability P eeas a function of energy, as predicted by the LMA-MSW solution of neutrino oscillations , is demonstrated by the curve in Fig. 3. neutrino mass oscillations. The question of the neutrino’s mass is an important one in much of modern astrophysics and particle physics, as knowing its mass will reveal fundamental information about the nature of the neutrino and will let us discover new things about the state of the early universe. 2. MASSLESS NEUTRINOSFile Size: KB. Neutrino-nucleus reaction cross sections are now evaluated rather accurately by shell-model (SM) or SM+RPA calculations based on recent advances in nuclear structure studies. Due to these achievements, reliable constraints on super-nova neutrino temperatures as well as neutrino oscillation parameters become possible. Supernova neutrino tempeatures are constrained from abundances of .
Abstract. A time projection chamber with a selenium double beta decay source as the central electrode has yielded a lower limit of × 10 20 years at the 68% confidence level for the two-neutrino half life of 82 Se. For the neutrinoless mode we find a corresponding limit of × 10 22 years, also at the 68% confidence level. However if this Majorana neutrino has SM interactions, its weak transition amplitudes squared are a factor 2 smaller than the ones observed for the physical neutrino. The detection of low. Let’s stress that in this case both the low energy matter content and the assumed symmetries provides an speciﬁc example of a theory which at low energy theory contains three light mass eigenstates with an eﬀective dim-5 interaction of the form () with The neutrino interaction eigenstates are denoted by ~. Nuclear Physics B () North-Holland, Amsterdam HEAVY Z BOSONS AND MAJORANA NEUTRINOS M.J. DUNCAN and Paul LANGACKER Department of Physics, University of Pennsylvania, Philadelphia, PA , USA Received 13 March Several extensions of the standard model predict the existence of additional Z bosons, which could possibly be in the .
"Proceedings of the fourth course of the International School of Exotic Atoms, held March April 6, , at the Ettore Majorana Center for Scientific Culture, Erice, Sicily, Italy"--Title page verso. Description: ix, pages: illustrations ; 25 cm. Contents: I The Electro-Weak Force at Low Energy.- Weak Interactions at Low Energy The fourth course of the International School of Physics of Exotic Atoms took place at the "Ettore Majorana" Center for Scien tific Culture, Erice, from March 31 to April 6, As tradition, exotic atoms have been a tool for studying elec tromagnetic, weak and strong interactions at low. The physical meaning of the rest mass of neutrino In the late 60's, physicists successfully unified the electromagnetic interaction and the weak interaction into the Electroweak Theory and received the Nobel Prize in physics afterward. The theory had predicted the mass of neutrino to be zero. Neutrino mass and gauge structure of weak interactions (Telemark, ). New York: American Institute of Physics, (OCoLC) Material Type: Conference publication, Internet resource: Document Type: Book, Internet Resource: All Authors / Contributors: V Barger; D Cline.