Electromagnetic neutrinos in laboratory experiments and astrophysics

Abstract

An overview of neutrino electromagnetic properties, which open a door to the new physics beyond the Standard Model, is given. The effects of neutrino electromagnetic interactions both in terrestrial experiments and in astrophysical environments are discussed. The experimental bounds on neutrino electromagnetic characteristics are summarized. Future astrophysical probes of electromagnetic neutrinos are outlined.Comment: 18 pages, 2 figures, Revised version, Annalen der Physik [Ann. Phys. (Berlin)] in press. arXiv admin note: substantial text overlap with arXiv:1403.634

Electromagnetic properties of massive neutrinos in low-energy elastic neutrino-electron scattering

“…[4][5][6]. In this section we briefly outline the general form of the electromagnetic interactions of Dirac and Majorana neutrinos.…”

“…[23]. In the case of millicharged massive neutrinos, electromagnetic gauge invariance implies that the diagonal electric charges e jj (j = 1, 2, 3) are equal [6]. It should be mentioned that the most stringent experimental constraints on the electric charge of the neutrino can be obtained from the neutrality of matter.…”

“…The development of our knowledge about neutrino masses and mixing [1][2][3] provides a basis for exploring neutrino properties and interactions beyond the standard model (BSM). In this respect, the study of nonvanishing electromagnetic characteristics of massive neutrinos is of particular interest [4][5][6]. It can help not only to shed light on whether neutrinos are Dirac or Majorana particles, but also to constrain the existing BSM theories and/or to hint at new physics.…”

Electromagnetic properties of neutrinos: a window to New Physics

“…It was shown that even tine values of the Majorana neutrino transition moments would probably be tested in future high-precision experiments with the astrophysical neutrinos. In particular, observations of supernova fluxes in the JUNO experiment (see [27][28][29]) may reveal the effect of collective spin-flavour oscillations due to the Majorana neutrino transition moment µ M ν ∼ 10 −21 µ B . There are indeed other new possibilities for neutrino magnetic moment visualization in extreme astrophysical environments considered recently [30,31].…”

Revisiting large neutrino magnetic moments

“…We have to take into account the naturalness condition on the squared mass difference ∆m 2 η = m 2 η 1 − m 2 η 2 , emerging from radiative corrections after symmetry breaking [29]: 10) where M V is the mass of the vector boson associated with the SU(2) ν symmetry breaking and α W is the electroweak fine-structure constant. Taking the experimental limits on the SU(3) L gauge boson masses [39] into consideration we set M V ∼ m η ∼ 5 TeV and get ∆m 2 η 7 · 10 5 GeV 2 .…”