Physics of Massive Neutrinos
The existence of an almost massless neutral particle (later on called neutrino by Fermi) was postulated by Pauli in 1932 to account for the continuous energy spectrum of the electrons emitted in nuclear (β decay. This particle was required to be a fermion in order to conserve angular momentum. Fermi incorporated this particle into a detailed theory of nuclear beta decay which could account for the observed shape of the electron energy distribution found in many nuclear beta decays. With availability of more experimental results, the original Fermi theory underwent many changes and finally culminated into a simple and elegant V — A theory [1, 2] which universally describes all the known (charged) weak interaction processes at low energy [3, 4, 5, 6]. The V — A theory is basically an effective theory which allows reliable calculations of weak interaction processes at energies ≪ O(100) GeV. The basic structure of this theory was later on generalized into a full fledged quantum theory based on ideas of spontaneously broken local gauge invariance . It became possible to unify the weak and electromagnetic interactions within this framework. The resulting theory is now known as the standard electroweak model.
Unable to display preview. Download preview PDF.
- E.D. Commins and P.H. Bucksbum, Weak interactions of leptons and quarks, Cambridge University Press (1983).Google Scholar
- C.W. Kim and A. Pevsner, Neutrinos in physics and astrophysics, Harwood Academic Publishers (1993)Google Scholar
- J. Bahcall et al, Solar neutrinos: The first thirty years, Perseus Publishing (1995).Google Scholar
- J. Bahcal, Neutrino astrophysics, Cambridge University Press (1989).Google Scholar
- W.C. Hexton and B. Holstein, hep-ph/9905257.Google Scholar
- A.S. Joshipura, hep-ph/0204305.Google Scholar
- Particle Data Group, K. Hagiwara et al, Phys. Rev. D66 (2002) 010001.Google Scholar
- The latest and earlier results and details of the experiments can be found at http://www-sk.icrr.u-tokyo.ac.jp
- The SAGE collaboration, astro-ph/0204245.Google Scholar
- The SNO collaboration, nucl-ex/0204008 and nucl-ex/0204009. See also http://www.sno.phy.queensu.ca/sno.
- A. Bandyopadhyay et al, hep-ph/00204286; V. Barger et al, hep-ph/0204253; J.N. Bahcall et. al, hep-ph/0204314; P.C. de-Hollanda and A. Yu. Smirnov, hep-ph/0205241; C.V.K. Baba, D. Indumathi and M.V.N. Murthy, Phys. Rev. D65 (2002) 073033.Google Scholar
- The LSND collaboration, hep-ex/0104049 and Phys. Rev. Lett. 81 (1998) 1774.Google Scholar
- The Karmen Collaboration, hep-ex/0203021 and E.D. Church et al, hep-ex/0203023.Google Scholar
- G.B. Gelmini and M. Roncadelli, Phys. Lett. 193 (1981) 297.Google Scholar
- Y. Koide, Nucl. Phys. Proc. Suppl. 111, 294 (2002) [hep-ph/0201250].Google Scholar
- A.Y. Smirnov and M. Tanimoto, Phys. Rev. D 55, 1665 (1997) [hep-ph/9604370].Google Scholar
- B. Brahmachari and A.S. Choubey, Phys. Lett B531 (192002) 99;Google Scholar
- A.S. Joshipura and P. Krastev, Phys. Rev. D50 (191994) 31.Google Scholar
- S. Goswami, Plenary talk at the International Symposium, PASCOS03, Bombay, India (2003), hep-ph/0307224.Google Scholar