583 research outputs found
Neutrino Physics with Dark Matter Experiments and the Signature of New Baryonic Neutral Currents
New neutrino states \nu_b, sterile under the Standard Model interactions, can
be coupled to baryons via the isoscalar vector currents that are much stronger
than the Standard Model weak interactions. If some fraction of solar neutrinos
oscillate into \nu_b on their way to Earth, the coherently enhanced elastic
\nu_b-nucleus scattering can generate a strong signal in the dark matter
detectors. For the interaction strength a few hundred times stronger than the
weak force, the elastic \nu_b-nucleus scattering via new baryonic currents may
account for the existing anomalies in the direct detection dark matter
experiments at low recoil. We point out that for solar neutrino energies the
baryon-current-induced inelastic scattering is suppressed, so that the possible
enhancement of new force is not in conflict with signals at dedicated neutrino
detectors. We check this explicitly by calculating the \nu_b-induced deuteron
breakup, and the excitation of 4.4 MeV \gamma-line in ^{12}C.
Stronger-than-weak force coupled to baryonic current implies the existence of
new abelian gauge group U(1)_B with a relatively light gauge boson.Comment: 20 pages, 5 figures. References added, inconsistent treatment of
neutrino oscillations corrected, conclusions unchange
On the Mass Eigenstate Composition of the 8B Neutrinos from the Sun
The present data of gallium experiments provide indirectly the only
experimental limit on the fraction of mass eigenstate for the B
neutrinos from the Sun. However, if to use the experimental data alone, the
fraction of and, consequently, still is allowed to
be varied within a rather broad range. The further experimental efforts are
needed to clear this point.Comment: 13 pages, 1 figure, 1 table. Corrected version, published in
JCAP04(2007)00
Interplay between collective effects and nonstandard interactions of supernova neutrinos
We consider the effect of non-standard neutrino interactions (NSI, for short) on the propagation of neutrinos through the supernova (SN) envelope within a three-neutrino framework and taking into account the presence of a neutrino background. We find that for given NSI parameters, with strength generically denoted by εij, neutrino evolution exhibits a significant time dependence. For |εττ|≳ 10−3 the neutrino survival probability may become sensitive to the θ23 octant and the sign of εττ. In particular, if εττ≳10−2 an internal I-resonance may arise independently of the matter density. For typical values found in SN simulations this takes place in the same dense-neutrino region above the neutrinosphere where collective effects occur, in particular during the synchronization regime. This resonance may lead to an exchange of the neutrino fluxes entering the bipolar regime. The main consequences are (i) bipolar conversion taking place for normal neutrino mass hierarchy and (ii) a transformation of the flux of low-energy νe, instead of the usual spectral swap
Neutrino Spin Transitions and the Violation of the Equivalence Principle
The violation of the equivalence principle (VEP) causing neutrino
oscillations is of current interest. We study here the possibility of not only
flavor oscillation but spin flavor oscillation of ultra high energy ( 1
PeV) neutrinos emanating from AGN due to VEP and due to the presence of a large
magnetic field ( 1 Tesla) in AGN. In particular we look at the resonance
spin flavor conversion driven by the AGN potential. Interesting bounds on the
transition magnetic moment of neutrinos may therefore be obtained.Comment: Latex, 12 pages, no figures. To appear in Journal of Physics G:
Nuclear and Particle Physics. Two references adde
Methods of approaching decoherence in the flavour sector due to space-time foam
In the first part of this work we discuss possible effects of stochastic
space-time foam configurations of quantum gravity on the propagation of
``flavoured'' (Klein-Gordon and Dirac) neutral particles, such as neutral
mesons and neutrinos. The formalism is not the usually assumed Lindblad one,
but it is based on random averages of quantum fluctuations of space time
metrics over which the propagation of the matter particles is considered. We
arrive at expressions for the respective oscillation probabilities between
flavours which are quite distinct from the ones pertaining to Lindblad-type
decoherence, including in addition to the (expected) Gaussian decay with time,
a modification to oscillation behaviour, as well as a power-law cutoff of the
time-profile of the respective probability. In the second part we consider
space-time foam configurations of quantum-fluctuating charged black holes as a
way of generating (parts of) neutrino mass differences, mimicking appropriately
the celebrated MSW effects of neutrinos in stochastically fluctuating random
media. We pay particular attention to disentangling genuine quantum-gravity
effects from ordinary effects due to the propagation of a neutrino through
ordinary matter. Our results are of interest to precision tests of quantum
gravity models using neutrinos as probes.Comment: 35 pages revtex, no figures, typos corrected in section II
Does the Borexino experiment have enough resolution to detect the neutrino flavor day-night asymmetry?
The Earth's density distribution can be approximately considered piecewise
continuous at the scale of two-flavor oscillations of neutrinos with energies
about 1 MeV. This quite general assumption appears to be enough to analytically
calculate the day-night asymmetry factor. Using the explicit time averaging
procedure, we show that, within the leading-order approximation, this factor is
determined by the electron density immediately before the detector, i.e. in the
Earth's crust. Within the approximation chosen, the resulting asymmetry factor
does not depend either on the properties of the inner Earth's layers or on the
substance and the dimensions of the detector. For beryllium neutrinos, we
arrive at the asymmetry factor estimation of about , which
is at least one order of magnitude beyond the present experimental resolution,
including that of the Borexino experiment.Comment: 16 pages, 3 figures; Talk given at the 17th International Seminar on
High Energy Physics "QUARKS'2012" (Yaroslavl, Russia, June 4-10, 2012); to
appear in the Proceedings volum
Effect of Coulomb collisions on time variations of the solar neutrino flux
We consider the possibility of time variations of the solar neutrino flux due
to the radial motion of the Earth and neutrino interference effects. We
calculate the time variations of the detected neutrino flux and the extent to
which they are suppressed by Coulomb collisions of the neutrino emitting
nuclei. To properly treat the collisions, it is necessary to simultaneously
include in our analysis all other significant physical decoherence effects: the
energy averaging and the averaging over the position of neutrino emission.
A simple and clear physical picture of the time dependent solar neutrino
problem is presented and qualitative coherence criteria are discussed. Exact
results for the detected neutrino flux and its time variations are obtained for
both the case of a solar neutrino line, and the case of the continuous neutrino
spectrum with a Gaussian shape of the energy response function of the neutrino
detector. We give accurate constraints on the vacuum mixing angle and the
neutrino masses required for flux time variations to not be suppressed.
Pac(s): 26.65.+t, 14.60.Pq, 96.60.JwComment: 43 pages, 8 figures, 4 appendices; changed title, MSW jump
probability formula and figure
Impact of right-handed interactions on the propagation of Dirac and Majorana neutrinos in matter
Dirac and Majorana neutrinos can be distinguished in relativistic neutrino
oscillations if new right-handed interactions exist, due to their different
propagation in matter. We review how these new interactions affect neutrino
oscillation experiments and discuss the size of this eventually observable
effect for different oscillation channels, baselines and neutrino energies.Comment: 26 pages, 5 figure
Decoherent Neutrino Mixing, Dark Energy and Matter-Antimatter Asymmetry
A CPT violating decoherence scenario can easily account for all the
experimental evidence in the neutrino sector including LSND. In this work it is
argued that this framework can also accommodate the Dark Energy content of the
Universe, as well as the observed matter-antimatter asymmetry.Comment: 6 pages, no figures, some typos corrected, and discussion modified
below eq (3), no effects on conclusion
Muon Flux Limits for Majorana Dark Matter Particles
We analyze the effects of capture of dark matter (DM) particles, with
successive annihilations, predicted in the minimal walking technicolor model
(MWT) by the Sun and the Earth. We show that the Super-Kamiokande (SK) upper
limit on excessive muon flux disfavors the mass interval between 100-200 GeV
for MWT DM with a suppressed Standard Model interaction (due to a mixing
angle), and the mass interval between 0-1500 GeV for MWT DM without such
suppression, upon making the standard assumption about the value of the local
DM distribution. In the first case, the exclusion interval is found to be very
sensitive to the DM distribution parameters and can vanish at the extreme of
the acceptable values.Comment: 20 pages, 12 figures. The revised version has minor addition (without
change of the result) as the following: 1) Comparison of our estimations with
analogous previous ones is included in the Figure 7; a paragraph regarding it
was added in Discussion. 2) The Introduction, Acknowledgements and References
have been a little extende
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