UHECR Signatures and Sources

Abstract. We discuss recent results on the clustering, composition and distribution of Ultra-High Energy Cosmic Rays (UHECR) in the sky; from the energy of several tens of EeV in the dipole anisotropy, up to the highest energy of a few narrow clusters, those of Hot Spots. Following the early UHECR composition records deviations from proton, we noted that the UHECR events above 40 EeV can be made not just by any light or heavy nuclei, but mainly by the lightest ones as He,D, Li,Be. The remarkable Virgo absence and the few localized nearby extragalactic sources, such as CenA, NGC 253 and M82, are naturally understood: lightest UHECR nuclei cannot reach us from the Virgo distance of twenty Mpc, due to their nuclei fragility above a few Mpc distances. Their deflection and smearing in wide hot spots is better tuned to the lighter nuclei than to the preferred proton or heavy nuclei candidate courier. We note that these lightest nuclei still suffer of a partial photodistruction even from such close sources. Therefore, their distruption in fragments, within few tens EeV multiplet chain of events, have been expected and later on observed by Auger collaboration, nearly a decade ago. These multiplet presences, strongly correlate with the same CenA, NGC253 sources. The statistical weight of such correlation is reminded. We conclude that the same role of NGC 253 clustering at lower energies could also feed the Auger dipole anisotropy at lower energy ranges, integrated by nearest Vela, Crab, LMC and Cas A contributes. In our present UHECR model, based on lightest nuclei in local volumes of a few Mpcs, closest AGN, Star-Burst or very close SNR are superimposing their signals, frozen in different epochs, distances and directions, feeding small and wide anisotropy. Possible tests to confirm, or untangle the current model from alternative ones, are suggested and updated.Comment: 4 pages, 4 figure

UHECR narrow clustering correlating IceCube through-going muons

The recent UHECR events by AUGER and the Telescope Array (TA) suggested that wide clusterings as the North and South, named Hot Spot, are related to near AGNs such as the one in M82 and Cen A. In the same frame since 2008 we assumed that the UHECR are made by light and lightest nuclei to explain the otherwise embarrassing absence of the huge nearby Virgo cluster, absence due to the fragility and the opacity of lightest nuclei by photo-dissociation from Virgo distances. Moreover UHECR map exhibits a few narrow clustering, some near the galactic plane, as toward SS 433 and on the opposite side of the plane at celestial horizons: we tagged them in 2014 suggesting possible near source active also as a UHE neutrino. Indeed since last year, 2015, highest IceCube trough-going muons, UHE up-going neutrino events at hundreds TeV energy, did show (by two cases over three tagged in North sky) the expected overlapping of UHE neutrinos signals with narrow crowding UHECR. New data with higher energy threshold somehow re-confirmed our preliminary proposal; new possible sources appear by a additional correlated UHE-neutrino versus UHE-neutrino and-or with narrow UHECR clustering events. A possible role of relic neutrino mass scattering by ZeV neutrino arised.Comment: 6 pages, 5 figure

Cascades in interdependent flow networks

In this manuscript, we investigate the abrupt breakdown behavior of coupled distribution grids under load growth. This scenario mimics the ever-increasing customer demand and the foreseen introduction of energy hubs interconnecting the different energy vectors. We extend an analytical model of cascading behavior due to line overloads to the case of interdependent networks and find evidence of first order transitions due to the long-range nature of the flows. Our results indicate that the foreseen increase in the couplings between the grids has two competing effects: on the one hand, it increases the safety region where grids can operate without withstanding systemic failures; on the other hand, it increases the possibility of a joint systems’ failure

Neutrino signals by Upward Tau airshowering at Earth horizons and by Muon airshowering at Moon shadows

International audienceNeutrinos are invisible, but their interactions with matter and their leptons signature leave an observable trace. Due to the huge atmospheric neutrino noise produced by cosmic ray rainpresent detectors are hidden deep in underground, as SK or IceCube detectors. At highest energy, atmospheric signal are found to be overcome by a new flavor signature. Because of it at those edges there is much hope for revealing highest energy neutrino as an astronomy, well above tens TeVs.We remind that the three neutrinos and antineutrinos flavors show different roles. Traces of GeVs-TeVs electrons radiate a lot, so they are short (on the order of meters) within solid matter.Muons, even if unstable, they radiate much less, so they are much more long life and penetrating (range of kilometers at TeVs eneregy in matter). These muons may be born inside a rock andescape from matter, as skimming from mountains; they may also decay over great distances, much larger than the size of Earth. In analogy, taus, the third and most unstable leptons, are hardlyformed from cosmic rays secondaries. Therefore they arise mainly from astrophysical neutrinos, that are democratically mixed during stellar and cosmic oscillating flights. Tau are also the most penetrating in principle but because they are extremely unstable, they are relevant only at PeVs energy edges. They may rise as a inner cascade and a later decay as a larger shower in icy: the so called double bang. The tau penetrability range and decay in rock, at PeV energy, is around 49 meters; the , onceescape in air , may decay in air-shower. For instance their escaping from a mountain or from the Earth, is amplified in a widest area and by richest secondaries as rare upgoing airshowers. Therefore, for more than twenty years they have been advocated and proposed as a new filtered neutrinos astronomy no longer hidden in underground detectors, free from most atmospheric noises. These are the signals searched by present ongoing experiments from mountains, valleys and from space: the tau airshowers. Nevertheless also muons at TeVs or higher energy can in principle decay in flight, but mainly onlyfrom the Moon distances. Their secondary electron may trace wide airshower on Earth atmosphere as gamma ones. Because the terrestrial and nearby magnetic fields, the bending begin to fadeabove 6.4 TeV; just above 61.2 TeVs the muons are mostly no longer able to decay in flight. Therefore, rarest gamma-like airshower in largest LHAASO like array, in the 6.4 TeVE 61.2 TeV windows, may be discovered in future years. The widest thousands of kilometer-size gamma array such as GRAND ARRAY can detect these trough going muons escaping from the Moon, decayingas electron or gamma on terrestrial airshowers.More energetic and fragmented decays can also rarely occur, from PeVs tau from the Moon. The corresponding solar shadow is opaque to neutrinos. But their skimming PeVs CRs could still shinemore likely muons, whose decay in flight may also soon rise as a gamma corona halo around our Sun, with a possibly already detectable signal in LHAASO

Where are the Ultra High Energy Cosmic Ray (UHECR) originated?

International audienceWe consider the recent results on UHECR (Ultra High Energy Cosmic Ray) composition and their distribution in the sky from ten EeV energy (the dipole anisotropy) up to the highest UHECR energies and their clustering maps: UHECR have been found mostly made by light and lightest nuclei. We summarized the arguments that favor a few localized nearby extragalactic sources for most UHECR as CenA, NG 253, M82. We comment also on the possible partial role of a few remarkable galactic UHECR sources. Finally we revive the eventual role of a relic neutrino eV mass in dark hot halo (hit by ZeV neutrinos) to explain the new UHECR clustering events centered around a very far cosmic AGN sources as 3C 454