Constraints on neutrino velocities revisited

Abstract

With a minimally modified dispersion relation for neutrinos, we reconsider the constraints on superluminal neutrino velocities from bremsstrahlung effects in the laboratory frame. Employing both the direct calculation approach and the virtual Z-boson approach, we obtain the generic decay width and energy loss rate of a superluminal neutrino with general energy. The Cohen-Glashow's analytical results for neutrinos with a relatively low energy are confirmed in both approaches. We employ the survival probability instead of the terminal energy to assess whether a neutrino with a given energy is observable or not in the OPERA experiment. Moreover, using our general results we perform systematical analyses on the constraints arising from the Super-Kamiokande and IceCube experiments.

Electroweak supersymmetry around the electroweak scale

“…properly. Especially, the discrepancies among the SM gauge couplings at the GUT scale are less than a few percents [68].…”

Neutrinos as Probes of Lorentz Invariance

“…In particular, coefficients leading to V ] > 1 in (11) can produceCerenkov emission of one or more particles [35,[82][83][84][85][86][87][88][89][90][91][92].Cerenkov radiation makes neutrinos lose energy, which distorts the spectrum in long-baseline experiments using accelerator and atmospheric neutrinos. This feature provides another method to search for Lorentz violation.…”

“…The observation of high-energy neutrinos after propagating a distance sets a lower value for the characteristic distortion distance ( ) = − /( / ) in the form < ( ). The determination of the characteristic distance for the spectral distortion caused by the isotropic Lorentz-violating operator of dimension four ( (4) of ) 00 is described in [82][83][84][85][86][87][88][89][90][91][92]. The general calculation including direction-dependent effects for operators of arbitrary dimension can be found in [35].…”

Testing Lorentz and CPT Invariance with Neutrinos

“…For instance, some coefficients in the neutrino velocity (6) can produce superluminal neutrinos, which could lose energy in the form of Cherenkov radiation [19,[50][51][52][53][54][55][56][57][58][59][60]. The determination of a characteristic energy-loss distance D(E) = −E/(dE/dx) due to Cherenkov radiation can be used to write the condition L < D(E), where L is the distance traveled by the neutrino [19].…”