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The conditions for a significant enhancement factor for the neutrino-anti-neutrino pair emission were established.
Instead, we shall follow here a different approach, which will eventually lead to the same kind of kinetic equation for the neutrino distribution.
As shown above, the parametric instability of the neutrino field could act as an amplifier of the direct and modified processes.
Cosmological neutrinos: can they contribute to molecular homochirality?
We see that the similarity is striking and that, again, the collective neutrino dynamics in a plasma strongly resembles that of the electrons.
If neutrinos are of sufficiently low mass, then it is expected that they probably contribute approximately the same amount.
The second is when the two possible neutrino helicity states are coupled by the electron plasma oscillations.
The collective coupling of neutrinos and anti-neutrinos in a dense plasma is considered.
The collective kinetic interaction of a neutrino distribution with electrostatic waves propagating in a dense plasma is considered.
Therefore, it is important to have a clear under standing of the ideal case of a monoenergetic neutrino beam.
As a final application, the case of a monoenergetic neutrino beam and the resulting neutrino-beam-plasma instability has been considered.
In steady state these two symmetric reactions lead to the emission of neutrinos and anti-neutrinos in equal number s and cool down the core of the star.
We use the known theoretical result of the split in energy of the two helicity states of an electron in the cosmic neutrino bath due to weak charged currents6,7.
Here, the replacement of the photon gas by the neutrino gas leads to the appearance of similar resonant kinetic interactions with the electron plasma waves, but also to specific features.
