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J. T. Peltoniemi

Publications and source records attributed to J. T. Peltoniemi.

7 recordsLinked to original sources
arXiv2000

Neutrino propagation in matter using the wave packet approach

We study the oscillations and conversions of relativistic neutrinos propagating in matter of variable density using the wave packet formalism. We show how the oscillation and coherence lengths are modified in comparison with the case of oscillations in vacuum. Secondly, we demonstrate how the equation of motion for two neutrino flavors can be formally solved for almost arbitrary density profile. We calculate finally how the use of wave packets alters the nonadiabatic level crossing probabilities. For the most common physical environments the corrections due to the width of the wave packet do not lead to observable effects.

hep-ph↗
arXiv1999

Testing neutrino instability with active galactic nuclei

Active galactic nuclei and gamma ray bursts at cosmological distances are sources of high-energy electron and muon neutrinos and provide a unique test bench for neutrino instability. The typical lifetime-to-mass ratio one can reach there is $τ/m\sim 500 Mpc/cE_ν\sim 500$ s/eV. We study the rapid decay channel $ν_i\toν_j+ϕ$, where $ϕ$ is a massless or very light scalar (possibly a Goldstone boson), and point out that one can test the coupling strength of $g_{ij}ν_iν_j$ down to $g_{ij}\lsim 10^{-8} eV/m$ by measuring the relative fluxes of $ν_{e}$, $ν_μ$ and $ν_τ$. This is orders of magnitude more stringent bound than what one can obtain in other phenomena, e.g. in neutrinoless double beta decay with scalar emission.

hep-ph↗
arXiv1997

Supernova Bounds on Resonant Active-Sterile Neutrino Conversions

We discuss the effects of resonant $ν_e \to ν_s$ and $\barν_e \to \barν_s$ ($ν_s$ is a sterile neutrino) conversions in the dense medium of a supernova. In particular, we assume the sterile neutrino $ν_s$ to be in the hot dark matter few eV mass range. The implications of such a scenario for the supernova shock re-heating, the detected $\barν_e$ signal from SN1987A and for the r-process nucleosynthesis hypothesis are analysed in some detail. The resulting constraints on mixing and mass difference for the $ν_e-ν_s$ system are derived. There is also an allowed region in the neutrino parameter space for which the r-process nucleosynthesis can be enhanced.

hep-ph↗
arXiv1995

Neutrino spin-flip effects in collapsing stars

We study the spin-flavor transitions of neutrinos in the magnetic fields of a collapsing star. For the neutrino mass squared difference (10^{-10} - 10) eV^2 the transitions take place in almost isotopically neutral region of the star, where the effective matter density is suppressed up to 3 - 4 orders of magnitude. This suppression is shown to increase the sensitivity of the neutrino bursts studies to the magnetic moment of neutrino by 1.5 - 2 orders of magnitude, and for realistic magnetic field the observable effects may exist for (2 - 3)10^{-14} Bohr magneton. In the isotopically neutral region the jumps of the effective potential exist which influence the probabilities of transitions. The experimental signatures of the spin-flavor transitions are discussed. In particular, in the case of direct mass hierarchy, the spin-flip effects result in a variety of modifications of the electron antineutrino spectrum. Taking this into account, we estimated the upper bounds on the magnetic moment from the SN1987A data. In the isotopically neutral region the effects of possible twist of the magnetic field on the way of neutrinos can be important, inducing distortion of the neutrino energy spectra and further increasing the sensitivity. However, if the total rotation angle is restricted the absolute change of probabilities is small.

hep-ph↗
arXiv1993

Reconciling Dark Matter, Solar and Atmospheric Neutrinos

We present models that can reconcile the solar and atmospheric neutrino data with the existence of a hot dark matter component in the universe. This dark matter is a quasi-Dirac neutrino whose mass $m_{DM}$ arises at the one-loop level. The solar neutrino deficit is explained via nonadiabatic conversions of electron neutrino to a sterile neutrino and the atmospheric neutrino data via maximal muon neutrino to tau neutrino oscillations generated by higher order loop diagrams. For $m_{DM} \sim 30$ eV the radiative neutrino decay can lead to photons that can ionize interstellar hydrogen. In one of the models one can have observable $ν_e$ to $ν_τ$ oscillation rates, with no appreciable muon neutrino oscillations at accelerator experiments. In addition, there can be observable rates for tau number violating processes such as $τ\to 3e$ and $τ\to e + γ$. In the other model one can have sizeable $ν_e$ to $ν_μ$ oscillation rates, as well as sizeable rates for muon number violating processes such as $μ\to e + γ$, $μ\to e + majoron$ and $μ\to 3e$.

hep-ph↗
arXiv1993

Massive neutrinos and electroweak baryogenesis

We show that certain models for neutrino masses that lead to the MSW explanation of the solar neutrino data and/or the hot dark matter component in the universe can also naturally allow for the successful generation of the cosmological baryon asymmetry at the electroweak scale. This follows either because the experimental Higgs boson mass limit is weakened due to the smaller production rate and the presence of sizeable invisible decays involving majoron emission, or due to the effect of additional electrically charged scalar bosons which substantially modify the condition for succesful baryogenesis.

hep-ph↗