Neutrino Light Research Articles

Bounds and prospects for the majoron model of left-handed neutrino masses

We analyze further implications of the existence of a massless boson - the Majoron - mainly coupled to left-handed neutrinos. Final lepton spectrum in pion leptonic decay is affected by Majoron bremsstrahlung, yielding a bound on Majoron-neutrino coupling from experimental data. Supernova dynamics is another issue discussed here. We address possible effects of the frequent neutrino-neutrino collisions, neutrino interconversion and light boson bremsstrahlung in neutrino scattering. In particular, we focus on the question of lepton number non-conservation. We find that deleptonization of the core and high-entropy collapse can occur, via a subtle interplay of neutrino interconversion and light boson bremsstrahlung. Then, we propose an unorthodox solution to the missing mass problem in the universe. Finally, we address the problem of galaxy formation, which appears in a new perspective within our model.

The neutrino radiation for a hot neutron star formation and the envelope outburst problem

With the equations of neutrino heat conductivity being used, the neutrino light curve is calculated for the spherically symmetrical collapse of an iron-oxygen 2M ⊙ star (Figure 1) up to the formation of a hot hydrostatically equilibrium neutron star. The total energy, radiated in the form of muon and electron neutrinos, is 5.8×1053 erg (0.16Mc 2). The mean neutrino particle energy is ∼12 MeV for all the time the collapse proceeds. The maximum neutrino luminosity value is equal to 3×1053 erg s−1. For a 10M ⊙ star collapse, the luminosity maximum 3×1054 erg s−1 takes place just at the moment of the formation of a black hole inside the collapsing star. The total radiated energy in this case is about 0.08Mc 2. The set of calculations, allowing for the deposition of momentum by means of neutrino-nuclear coherent scattering, brings us to a conclusion that the envelope outburst is only possible if the scattering cross-section is 50 times larger than the value experimentally accepted (inequality 20)).