898 research outputs found
Linearized flavor-stability analysis of dense neutrino streams
Neutrino-neutrino interactions in dense neutrino streams, like those emitted
by a core-collapse supernova, can lead to self-induced neutrino flavor
conversions. While this is a nonlinear phenomenon, the onset of these
conversions can be examined through a standard stability analysis of the
linearized equations of motion. The problem is reduced to a linear eigenvalue
equation that involves the neutrino density, energy spectrum, angular
distribution, and matter density. In the single-angle case, we reproduce
previous results and use them to identify two generic instabilities: The system
is stable above a cutoff density ("cutoff mode"), or can approach an asymptotic
instability for increasing density ("saturation mode"). We analyze multi-angle
effects on these generic types of instabilities and find that even the
saturation mode is suppressed at large densities. For both types of modes, a
given multi-angle spectrum typically is unstable when the neutrino and electron
densities are comparable, but stable when the neutrino density is much smaller
or much larger than the electron density. The role of an instability in the SN
context depends on the available growth time and on the range of affected
modes. At large matter density, most modes are off-resonance even when the
system is unstable.Comment: 19 pages, 8 figures, revtex4 forma
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
Field-induced axion emission via process in plasma
The annihilation into axion is investigated in a plasma and
an external magnetic field. This process via a plasmon intermediate state has a
resonant character at a particular energy of the emitted axion. The emissivity
by is compared with the axion cyclotron emissivity.Comment: 8 pages, latex, 4 PS figure
Light sterile neutrino production in the early universe with dynamical neutrino asymmetries
Light sterile neutrinos mixing with the active ones have been recently
proposed to solve different anomalies observed in short-baseline oscillation
experiments. These neutrinos can also be produced by oscillations of the active
neutrinos in the early universe, leaving possible traces on different
cosmological observables. Here we perform an updated study of the neutrino
kinetic equations in (3+1) and (2+1) oscillation schemes, dynamically evolving
primordial asymmetries of active neutrinos and taking into account for the
first time CP-violation effects. In the absence of neutrino asymmetries,
eV-mass scale sterile neutrinos would be completely thermalized creating a
tension with respect to the CMB, LSS and BBN data. In the past literature,
active neutrino asymmetries have been invoked as a way to inhibit the sterile
neutrino production via the in-medium suppression of the sterile-active mixing
angle. However, neutrino asymmetries also permit a resonant sterile neutrino
production. We find that if the active species have equal asymmetries L, a
value |L|=10^{-3} is required to start suppressing the resonant sterile
production, roughly an order of magnitude larger than what previously expected.
When active species have opposite asymmetries the sterile abundance is further
enhanced, requiring an even larger |L|\simeq 10^{-2} to start suppressing their
production. In the latter case, CP-violation (naturally expected) further
exacerbates the phenomenon. Some consequences for cosmological observables are
briefly discussed: for example, it is likely that moderate suppressions of the
sterile species production are associated with significant spectral distortions
of the active neutrino species, with potentially interesting phenomenological
consequences especially for BBN.Comment: (v2: 22 pages, 10 eps figures. Revised version. Typos removed,
reference updated. Matches the version published on PRD.
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
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
Oscillations of high energy neutrinos in matter: Precise formalism and parametric resonance
We present a formalism for precise description of oscillation phenomena in
matter at high energies or high densities, V > \Delta m^2/2E, where V is the
matter-induced potential of neutrinos. The accuracy of the approximation is
determined by the quantity \sin^2 2\theta_m \Delta V/2\pi V, where \theta_m is
the mixing angle in matter and \Delta V is a typical change of the potential
over the oscillation length (l \sim 2\pi/V). We derive simple and physically
transparent formulas for the oscillation probabilities, which are valid for
arbitrary matter density profiles. They can be applied to oscillations of high
energy (E > 10 GeV) accelerator, atmospheric and cosmic neutrinos in the matter
of the Earth, substantially simplifying numerical calculations and providing an
insight into the physics of neutrino oscillations in matter. The effect of
parametric enhancement of the oscillations of high energy neutrinos is
considered. Future high statistics experiments can provide an unambiguous
evidence for this effect.Comment: LaTeX, 5 pages, 1 figure. Linestyles in the figure corrected to match
their description in the caption; improved discussion of the accuracy of the
results; references added. Results and conclusions unchange
Neutrino mass hierarchy and octant determination with atmospheric neutrinos
The recent discovery by the Daya-Bay and RENO experiments, that \theta_{13}
is nonzero and relatively large, significantly impacts existing experiments and
the planning of future facilities. In many scenarios, the nonzero value of
\theta_{13} implies that \theta_{23} is likely to be different from \pi/4.
Additionally, large detectors will be sensitive to matter effects on the
oscillations of atmospheric neutrinos, making it possible to determine the
neutrino mass hierarchy and the octant of \theta_{23}. We show that a 50 kT
magnetized liquid argon neutrino detector can ascertain the mass hierarchy with
a significance larger than 4 sigma with moderate exposure times, and the octant
at the level of 2-3 sigma with greater exposure.Comment: 4 pages, 4 figures. Version published in Phys. Rev. Let
Flavored Quantum Boltzmann Equations
We derive from first principles, using non-equilibrium field theory, the
quantum Boltzmann equations that describe the dynamics of flavor oscillations,
collisions, and a time-dependent mass matrix in the early universe. Working to
leading non-trivial order in ratios of relevant time scales, we study in detail
a toy model for weak scale baryogenesis: two scalar species that mix through a
slowly varying time-dependent and CP-violating mass matrix, and interact with a
thermal bath. This model clearly illustrates how the CP asymmetry arises
through coherent flavor oscillations in a non-trivial background. We solve the
Boltzmann equations numerically for the density matrices, investigating the
impact of collisions in various regimes.Comment: 41 pages, 7 figures. v2: references added, minor corrections and
clarification
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