Neutrino Flavor Conversions in High-Density Astrophysical and Cosmological Environments
Abstract
:1. Introduction
2. Equations of Motions
3. Flavor Conversions in the Early Universe
Active–Sterile Neutrino Oscillations
4. Flavor Conversions in Core-Collapse Supernovae
4.1. MSW Resonances
4.2. Collective Effects
4.2.1. Slow Flavor Conversions
- Multi angle effects [171,172,173,174]. When the flavor asymmetries are mild the phase dispersion induced by different propagation lengths of neutrinos can smear or completely remove the effects of the spectral splits, eventually leading to complete decoherence, i.e., all flavors are equilibrated up to lepton number conservation.
- Sponteneous breaking of azimuthal [181,182,183,184,185], spatial homogeneity [186,187,188,189,190,191,192], and stationarity [193,194]. It has been realized that the symmetries used as initial conditions of neutrino emission (azimuthal symmetry, spatial homogeineity, stationarity) are spontaneously broken during neutrino propagation. This leads to new instabilities that can develop in both mass orderings, but they are in general suppressed when the matter potential is dominating. Nevertheless, it has been shown [193,194] that self-interacting neutrinos can generate a pulsating solution with a frequency that effectively compensates the phase dispersion associated with the large matter term, lifting the suppression and making collective oscillations possible deep inside the supernova. However, because the matter potential changes during neutrino propagation, it is not clear whether a flavor wave with a specific pulsation can have enough time to grow and lead to significant flavor conversions. The presence of turbulent variations of the matter potential may introduce a coupling among flavor waves with different k, so making it more likely to have an instability even when neutrinos are propagating away in a supernova [195].
- Neutrino halo effect [196,197,198,199,200,201]. Neutrinos are not completely free-streaming after the neutrinosphere and even a small fraction of scattering neutrinos can produce a small “neutrino halo”. Such inward-going neutrinos can modify the outcome of conversions and the shape of spectral splits, if present, but, according to the latest simulations, the effects have been found to be relatively small.
4.2.2. Fast Flavor Conversions
- Proto-neutron star [220,221,222]. The physical origin of the crossings is a strong convective activity happening in the proto-neutron star, which can generate large amplitude modulations in the spatial distributions of and number densities. The physical implications are not very clear due to the nearly equal distributions of neutrinos and antineutrinos of all flavors.
- Neutrino decoupling region [221,223,224]. Their existence can be explained by the neutron richness of matter, which induces a later decoupling of with respect to and, thus, a more forward peaked angular distributions of . Another possibility is the presence of LESA [225,226,227,228], i.e., an asymmetric emission of lepton number, or other phenomena [228].
- Free streaming regime [229,230,231]. Crossings can be generated by neutrino backward scatterings off heavy nuclei and their size seems to get larger for smaller radial distances [229,230,231]. Such crossings are ubiquitous in the pre-shock region, but they can also occur in the post-shock region. In the former case, there is hardly an impact on astrophysical processes and on the detection at Earth [232,233], both because of the slower growth rates of the instabilities and the very small size of the amount of conversions expected. On the other hand, the instabilities developing in the post-shock region might produce an observable effect.
- Propagation of the power of the instability to small angular scales [236,237,238,239,240,241]. During its evolution, the power of a fast instability is moved from large scales to small ones in momentum space, accelerating the decoherence of the system (and the equilibration of flavors) [236,237,238,239,240,241]. Moreover, when considering a coarse-graining over space, fast conversions seem to eventually reach a steady state [239,240,241]. In particular in [240] an approximate analytical formula has been derived for calculating the amount of decoherence reached in fast conversions and, thus, the final amount of flavor conversions. This formula depends on the propagation angle of neutrinos and on the initial asymmetry between the total number of neutrinos and antineutrinos. If the asymmetry is extremely small, as expected for the crossings generated by backward scattering of neutrinos in the free streaming regime, then the amount of flavor conversions is expected to be negligible, as confirmed in [232,233]. In [240] the analytical formula is independent from the type of perturbation used to seed the flavor instabilities. However, in [241] a distinction is made between localized and random seeds. In the first case a coherent behavior in the space and momentum evolution of the flavor wave is retained for a longer time. The difference between [240] and [241] can be associated to heterogeneous numerical methods employed for calculating spatial derivatives.
- Spontaneous symmetry breaking [242]. As also happens to slow conversions, in the context of fast ones there is also a spontaneous breaking of the symmetries imposed in the initial conditions. This has been shown to happen for the azimuthal symmetry in [242] and in [243], though in the second reference it was not explicitly stated in the conclusions.
- Dependence on neutrino energy [244]. It has been proposed that the outcome of fast conversions depends on the size of the mass differences between mass eigenstates and on their ordering [244]. This claim has been criticized in [245] where only a modest dependence has been observed. However, the first simulation has been performed considering an homogeneous system, whereas the second has also taken into account the spatial evolution.
- Impact of inelastic collisions [245,246,247,248,249]. Since the conditions for fast conversions have been found even in locations where neutrinos are still partially or completely coupled to the plasma, there have been a few studies implementing collisions in numerical simulations. In this context, the authors of [247,248] reported the possibility of enhancement of flavor conversions, assuming only evolution in time. On the other hand, in [245,249] both time and space evolution have been taken into account and it was observed that collisions might cause flavor depolarization, thus suppressing conversions, but that a much larger mean free path than expected is required in order for this happen. This is in agreement to what found in [246], where the role of collisions in the generation of crossing has been also pointed out.
- Dependence on the number of neutrino species [242,243]. Considering six neutrino species the crossings and, thus, fast instabilities can occur in one (or more) of the three sectors and then propagate to other ones [243]. Moreover, even considering the distributions of to be the same, the outcome of flavor conversions is different [242] with respect to what obtained by using only the equation of motions for three species, as usually done in literature.
5. Fast Flavor Conversions in Compact Binary Mergers
6. Conclusions and Future Perspectives
Author Contributions
Funding
Data Availability Statement
Acknowledgments
Conflicts of Interest
1 | In order to include the correction due to the non-local nature of the Z boson propagator which mediate forward scattering on neutrinos of the same species. |
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Capozzi, F.; Saviano, N. Neutrino Flavor Conversions in High-Density Astrophysical and Cosmological Environments. Universe 2022, 8, 94. https://doi.org/10.3390/universe8020094
Capozzi F, Saviano N. Neutrino Flavor Conversions in High-Density Astrophysical and Cosmological Environments. Universe. 2022; 8(2):94. https://doi.org/10.3390/universe8020094
Chicago/Turabian StyleCapozzi, Francesco, and Ninetta Saviano. 2022. "Neutrino Flavor Conversions in High-Density Astrophysical and Cosmological Environments" Universe 8, no. 2: 94. https://doi.org/10.3390/universe8020094
APA StyleCapozzi, F., & Saviano, N. (2022). Neutrino Flavor Conversions in High-Density Astrophysical and Cosmological Environments. Universe, 8(2), 94. https://doi.org/10.3390/universe8020094