Past and recent observations suggest that many planetary mass or dwarf planet objects may exist in the outer Solar System. Gravitational perturbations may occasionally bring some of them into the inner Solar System. The early, rare collision between the early Earth and a Mars sized body is generally invoked to explain the formation of the Moon. More probable than a direct impact, are grazing or near Earth flybys of similar objects. Such passages may have left strong tidal signatures: giant waves, large volcanic episodes, sea regressions, coherent meteor showers, and major climatic perturbations. These mechanisms could have contributed to several major biological mass extinctions over the past 600 million years, as suggested by peculiar correlations in the geological record. Similar events may have occurred several times during the earlier history of Earth. Accretion of mini planets by largest planets and in particular by the Sun may also have occurred many more times over the last four billion years. Possibly producing additional temperature variations on planets and Earth.

UHECR are evalueted in the frame role of different nuclei composition. Most of the past and present models are considering proton or iron as their main currier. Some attention has been paid to the role of the UHECR light nuclei in recent years. We update here the lightest nuclei UHECR model, able to explain the nearest AGN or Star Burst sources with the few observed Hot Spot clustering in AUGER and TA array data. Any additional components of the heaviest nuclei with the highest energy, more bent and smeared, may also fit recent AUGER and TA homogeneous records at those energy edges.

The SS433 is a well-known binary system with an internal black hole, which is stripping mass from an orbiting companion of ten solar masses, at a hundred of light-seconds away. The black hole and its accretion disk fuel a thin precessing jet, whose spirals are well-observed. Surprisingly, disconnected gamma-ray tails have recently been discovered by H.E.S.S., HAWC and LHAASO, hundreds of light-years away and with energies of tens of TeV. We suggest that tens PeV neutron burst jets were ejected from the SS433 system over the past century. These beams of ultra high-energy PeVatron neutrons, by their in-flight beta decay and Inverse Compton scattering, could be the source of the enigmatic, distant and disconnected tens of TeV gamma-ray beams. These ultra-relativistic PeV neutron jets could have been formed during one of the system's rare and intense tidal eruptions, when tens of PeV protons collide CV October 2025 with thermal ultraviolet photons, creating delta resonances. Their decay into secondary neutron beams of tens of PeV is well consistent with observations. Alternative models appear uncompetitive.

Cosmic rays with energies of tens of TeV and above, skimming the Sun, could fragment into pions. The resulting gamma photons and muons, as well as subsequent electron pairs, will reach us in the form of gamma or electromagnetic air-showers , gamma-like air-showers on Earth. Their multiple presence may soon be observed and disentangled by the LHAASO telescope array.

The ultra-high-energy cosmic ray (UHECR) puzzle is reviewed under the hints of a few basic results: clustering, anisotropy, asymmetry, bending, and composition changes with energies. We show how the lightest UHECR nuclei from the nearest AGN or Star-Burst sources, located inside a few Mpc Local Sheets, may explain, at best, the observed clustering of Hot Spots at tens EeV energy. Among the possible local extragalactic candidate sources, we derived the main contribution of very few galactic sources. These are located in the Local Sheet plane within a distance of a few Mpc, ejecting UHECR at a few tens of EeV energy. UHECR also shine at lower energies of several EeV, partially feeding the Auger dipole by LMC and possibly a few nearer galactic sources. For the very recent highest energy UHECR event, if a nucleon, it may be explained by a model based on the scattering of UHE ZeV neutrinos on low-mass relic neutrinos. Such scatterings are capable of correlating, via Z boson resonance, the most distant cosmic sources above the GZK bound with such an enigmatic UHECR event. Otherwise, these extreme events, if made by the heaviest composition, could originate from the largest bending trajectory of heaviest nuclei or from nearby sources, even galactic ones. In summary, the present lightest to heavy nuclei model UHECR from the Local Sheet could successfully correlate UHECR clustering with the nearest galaxies and AGN. Heavy UHECR may shine by being widely deflected from the Local Sheet or from past galactic, GRB, or SGR explosive ejection.

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. Such lower energy anisotropy could be fed and 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.

Skimming Cosmic Rays on the external Solar atmosphere can be showering in gamma, electron and energetic muon pairs. Such secondaries of TeV or higher energy could reach Earth along a thin frontal solar ring. The skimming gamma and electron rays are abundant, but originated in a very thin layer of the solar atmosphere, disturbed and obstacled in their propagation by solar corona fields and plasma scattering. On the contrary, secondary TeVs-PeVs muons are much rare, but are much more penetrating : they may escape from deeper solar edges along large cord distances, forming a thicker solar ring areas, shining brighter towards our Earth. Being muons of opposite charges, their trajectories are splitted in a twin ring of muons signals that should finally exit the Sun, decays in flight, reaching array detectors on Earth. These muons and their decay in electron pairs, even partially deflected up a few TeVs, must lead to rare gamma-like, air-showers, in LHAASO array detector, falling inside or around the same solar shadows. These rare gamma-like airshowers must be soon disentangled and observable within an energy range of a few up to tens TeV energy. A more rare, more exciting, signal must also occur from the entire lunar surface or disk, by upward escaping TeVs muons toward the Earth, made by tens TeV muon astrophysical neutrinos , interacting in a few kilometer lunar crust depth, shining around a 6 − 60 TeV energy windows, as above, as detectable electron air-shower. Such a lunar mass volume, as a calorimeter for astrophysical neutrinos, is at least a million times larger than the IceCube one, but their arrival solid angle is extremely small. Therefore this lunar disk area signals will be hardly observable in present LHAASO, even within several years or decades. However future larger area, LHAASO like arrays, might be opening the road to a guaranteed lunar induced neutrino muon Astronomy. The first expected solar (and lunar) air-shower rate and geometry in their LHAASO shadows are described.

Icecube neutrino detector a cubic kilometer in South Pole, traces energetic TeVs-PeVs neutrino signals by their cascades or better by their tracks inside its icy volume. Cascades, explosive spherical showers in icy, are mostly for electron or tau or neutral current, tracks are made by muons. High energy tau tracks might show a birth place cascade and a second decay tau shower, allowing a peculiar directional track. In general hundreds TeVs-PeVs Cascades show very poor directionality. Therefore they are nearly blind to disentangle the source event. Therefore we suggest to neglect such cascades in future Gen-2 Icecube. Indeed the most interesting signals are the tens TeVs up PeVs muon upgoing tracks, either born inside, HESE, or outside Icecube: the trought going muon tracks. These ones are more abundant at ultra high energy (UHE) regimes because their interactions is outside the Icecube, mainly in the wider volume of dense rock around and below the Icecube volume. Such several kilometers tracks offer the most energetic and precise neutrino astronomy. Moreover highest tens TeV or PeVs neutrinos become opaque to the Earth radius. Therefore they are arriving mainly as up-going nearly horizontal tracks, because they are crossing only short Earth cords. In consequence we suggest an upgrade Muon Icecube detector by a widest kilometers spaced concentric spiral array rings (around old Icecube), each arm nearly a kilometer far from the other, leading to the largest and widest array net (for any given string number). Such wider (km) empty array volumes, like a sponge, may better amplify, almost quadratically, the observed mass volume, in comparision to a more dense but homogeneous volumetric cubic one (at 240 or 330 meters distance among strings) as the Icecube Gen-2 project. In our first approximation one may obtain an increased cubic volume reaching about 50 times the kilometer Icecube array, by a shell like spiral volume or a honeycomb cell net, leading not to a few rare (hundred TeV energy) event a year but to many tens or even a hundred of such neutrino tracks each year, running toward a more statistical rich Astronomy

We consider the recent results on UHECR (Ultra High Energy Cosmic Ray), clustering, composition, distribution in the sky, from the energy of several EeV with the dipole anisotropy up to the highest ones. We have suggested since 2008 and we reconfirm here that UHECR at 40 up to 70 EeV are mostly made by light and lightest nuclei. The remarkable Virgo absence and the few localized nearby extragalactic sources as CenA, NG 253, M82 may be well understood by the lightest nuclei fragility and opacity within Mpc distances. We comment also on the role of a few galactic UHECR sources at ten EeV that may be partially feeding the Auger dipole UHECR anisotropy. The recent anisotropy in the UHECR spectral composition of lightest and heavy nuclei, outside and along the galactic plane, could also be a first confirmation of our previous claims (2012). The interplay of the heavier and most energetic UHECR galactic nuclei with the mainly local (Mpcs) extragalactic signals ruled by lightest nuclei, seems to fit the main pieces of UHECR puzzle.

Neutrinos 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 rain present 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 and escape 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 hardly formed 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 tau, once escape 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 only from 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 fade above 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 - 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, decaying as 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 shine more 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.

The CoVid-19 is spreading pandemically all over the world. A rapid defeat of the pandemic requires carrying out on the population a mass screening, able to separate positive from negative cases. Such a cleaning will free a flow of productive population. The current rate and cost of testing, performed with the common PCR (polymerase chain reaction) method and with the available resources, is forcing a selection of the subjects to be tested. Indeed, each one must be examined individually at the cost of precious time. Moreover, the exclusion of potentially positive individuals from screening induces health risks, a broad slowdown in the effort to curb the viral spread, and the consequent mortality rates. We present a new procedure, the Purified by Unified Resampling of Infected Multitudes, in short Purim, able to untangle any massive candidate sample with inexpensive screening, through the cross-correlated analysis of the joint speciments. This procedure can reveal and detect most negative patients and in most cases discover the identity of the few positives already in the first or few secondary tests. We investigate the the two-dimensional correlation case in function of the infection probability. The multi-dimensional topology, the scaled Purim procedure are also considered. Extensive Purim tests may measure and weight the degree of epidemic: their outcome may identify focal regions in the early stages. Assuming hundreds or thousand subjects, the saving both in time and in cost will be remarkable. Purim may be able to filter scheduled flights, scholar acceptance, popular international event participants. The optimal extension of Purim outcome is growing as the inverse of the epidemia expansion. Therefore, the earlier, the better.

IceCube Neutrino Astronomy is considered. The tau neutrino flavor paucity and the asymmetry for the tracks suggest a dominant atmospheric charm noise. The correlated cascades and tracks asymmetry with relevant statistics enforce the charm noise dominance in the data. The charm signal may explain at once the absence of correlation for the tracks data with the galactic plane and with known brightest gamma sources.

Last two years high energy neutrino data are studied.The two recent tau neutrino double bang candidate are discussed within their detectability, noise and expected rate.The neutrino flavor distribution mainly favoring equal electron and muon presence, is reminded.The angular distribution of highest muon neutrino tracks is analyzed.Their horizontal strong anisotropy and their remarkable up-down asymmetry, with the absence of clustering, is noticed.The main persistent missing of astrophysical X,gamma sources (as GRB and AGN flaring source) and all the above signatures led us to suggest a dominance of prompt charmed (atmospheric) events able to pollute, to smear and to hide any minor astronomical presence.

The largest solar flare have been recorded in gamma flash and hard spectra up to tens GeV energy. The present building and upgrade of Hyper- Kamiokande (HK) in Japan and Korea, (as well as Deep Core, PINGU) Megatons neutrino detectors do offer a novel way to detectable trace of solar flares: their sudden anti-neutrino (or neutrino) imprint made by proton scattering and pion decays via Delta resonance production on solar corona foot-point. These signals might be observable at largest flare by HK via soft spectra up to tens-hundred MeV energy and by IceCube-PINGU at higher, GeVs energies. We show the expected rate of signals for the most powerful solar flare occurred in recent decades extrapolated for future Megaton detectors. The neutrino solar flare detection with its prompt alarm system may alert astronauts on space journey allowing them to hide themselves into inner rocket container surrounded by fuel or water supply. These container walls are able to defend astronauts from the main lethal (the dominant soft component) radiation wind due to such largest solar flares.

The exciting development of gravitational wave (GW) astronomy in the correlation of LIGO and VIRGO detection of GW signals makes possible to expect registration of effects of not only binary black hole (BH) coalescence but also binary neutron star (NS) merging accompanied by electromagnetic (gamma ray burst; GRB) signal. Here we consider the possibility that an NS, merging in an NS–NS or NS–BH system might be (soon) observed in correlation with any LIGO–VIRGO GWs detection. We analyze as an example the recent case of the short GRB170817A observed by Fermi and integral. The associated optical transient (OT) source in NGC4993 implies a rare near source, a consequent averaged large rate of such events (almost) compatible with expected NS–NS merging rate. However the expected beamed GRB (or short GRB) may be mostly aligned to a different direction than ours. Therefore, even soft GRB photons, spread more than hard ones, might be hardly able to shower to us. Nevertheless, a prompt spiraling electron turbine jet in largest magnetic fields, at the base of the NS–NS collapse, might shine by its tangential synchrotron radiation in spread way with its skimming photons shining in large open disk. The consequent solid angle for such soft disk gamma radiation may be large enough to be nevertheless often observed.

Since 2013, the highest energy IceCube cascade showers overcame the common muon neutrino tracks. This fast flavor changes, above few tens TeV, has been indebt to the injection of the long searched astrophysical neutrino. However for what concern the recent published ICECUBE 54 neutrino, High Energy Starting Events, (HESE) in 2016, as well as the most recent ones of 82 and 103 IceCube events (2017-2018) and the several dozens of thorough-going muon tracks formed around the IceCube, none of them are pointing or clustering toward any expected x, gamma or radio sources: no one in connection to GRB, no toward active BL Lac, neither to AGN source in Fermi catalog. No clear correlation with nearby mass distribution (Local Group), nor with galactic plane. Withal, there have not been any record of the expected double bang due to the tau neutrino birth and decay among several events above 200 TeV energy (we are disregarding for a moment the most celebrated recent first correlated, but unique, muon track and the recent two tau possible identification); no any self-clustering events at tens TeV energy raised in most recent searches. Furthermore, there is a tension between the internal HESE event spectra power index and the external thorough-going muon tracks one. As we will show at the conclusions a more mundane (but a bit more abundant) prompt charmed atmospheric neutrino component may pollute and rule the data, explaining most of the present enlisted IceCube puzzles. We review the last HESE event data shown in early and in most recent papers (and talks in Neutrino 2018) making the case for the simplest conclusions. We believe that most astrophysical neutrino signals are still hidden below the ashes of these new, anyway discovered, prompt atmospheric noise.

The Sun albedo of Cosmic Rays (CRs) at GeVs energy has been discovered recently by the FERMI satellite. They are traces of atmospheric CRs hitting solar atmosphere and reflecting skimming gamma photons. Even if relevant for astrophysics, as being a trace of atmospheric solar CR noises they cannot offer any signal of neutrino astronomy. On the contrary, the Moon with no atmosphere, may become soon a novel filtering calorimeter and an amplifier of energetic muon astronomical neutrinos (at TeV up to hundred TeVs energy); these lepton tracks leave an imprint in their beta decay while in flight to Earth. Their TeV electron air-shower are among the main signals. Also, a more energetic, but more rare, PeV up to EeV tau lunar neutrino events may be escaping as a tau lepton from the Moon: [Formula: see text] PeV secondaries, then, may be shining on Earth’s atmosphere in lunar shadows in a surprising way. One or a few gamma air-shower events inside the Moon shadows may occur each year in near future Cherenkov telescope array (CTA) or large high altitude air shower observatory (LHAASO) TeV gamma array detector, assuming a nonnegligible astrophysical TeV up to hundred TeV neutrino component (with respect to our terrestrial ruling atmospheric ones); these signals will open a new wonderful passe-partout keyhole for neutrino, been seen along the Moon. The lunar solid angle is small and the muon or tau expected rate is rare, but with the future largest tau radio array as the giant radio array for neutrino detection (GRAND), one might well discover such neutrino imprint.

Since 2013 IceCube cascade showers sudden overabundance have shown a fast flavor change above 30-60 TeV up to PeV energy. This flavor change from dominant muon tracks at TeVs to shower events at higher energies, has been indebted to a new injection of a neutrino astronomy. However the recent published 54 neutrino HESE, high energy starting events, as well as the 38 external muon tracks made by trough going muon formed around the IceCube, none of them are pointing to any expected X-gamma or radio sources: no one in connection to GRB, no toward active BL Lac, neither to AGN source in Fermi catalog. No clear correlation with nearby mass distribution (Local Group), nor to galactic plane. Moreover there have not been any record (among a dozen of 200 TeV energetic events) of the expected double bang due to the tau neutrino birth and decay. An amazing and surprising unfair distribution in flavor (suppressing tau) versus an expected democratic one. Finally there is not a complete consistence of the internal HESE event spectra and the external crossing muon track ones. Moreover the apparent sudden astrophysical neutrino flux rise at 60 TeV might be probably also suddenly cut at a few PeV in order to hide the (unobserved , yet) Glashow resonance peak at 6.3 PeV. A more mundane prompt charmed atmospheric neutrino component may explain most of the IceCube puzzles. If in this near future, 2017-2018, ICECUBE does not discover any tau neutrino signals somewhere (by double bang) there are a list of consequences to face. These missing correlations and in particular the tau signature absence force us to claim. as in a famous Martini spot: No Tau? No Astronomy.