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The understanding of microquasars in our galaxy is one of the frontiers of high energy astrophysics. Their models are based on a capturing mass Black Hole, with a nearby spiraling binary companion star. The companion star mass feeds the accretion disk around the Black Hole. This energy also fuels an orthogonal precessing X gamma jets. The spiral precessing tail of such microquasars, as the SS433 system, is due to an ultra-relativistic jet, spraying nucleons and electrons at relativistic speeds. The up-down jet is observable in radio, X, gamma spectra. Its long spirals are spread and diluted within a light-year distance. The source is inside the W50 supernova remnant nebula , whose asymmetry reflects the past and present role of the SS433 jet. Very recently HESS, HAWC discovered, surprisingly at a much far disconnected distance from the SS433, the resurgence of a twin gamma beam tail. Nearly 75 years light distance far away from the same inner jet source. The recent standard model is based on an accelerating shock wave which reaccelerates, the resurgence of a PeV nucleon beam and its TeV secondaries. The surprising recollimation of this TeV beam jet is difficult to be accepted, in the assumption of a planarlike Fermi shock wave model. Here we discuss an alternative framework based on known high energy nuclear physics, capable to simultaneously explaining both the disconnected and the aligned hard TeV jet appearance. Several consequences, that might also be able to validate the model, are considered., Comment: 10 pages, 2 figures

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., Comment: 26 pages. 10 figures, Universe Journal, https://doi.org/10.3390/universe10080323

Interactive coding allows two parties to conduct a distributed computation despite noise corrupting a certain fraction of their communication. Dani et al.\@ (Inf.\@ and Comp., 2018) suggested a novel setting in which the amount of noise is unbounded and can significantly exceed the length of the (noise-free) computation. While no solution is possible in the worst case, under the restriction of oblivious noise, Dani et al.\@ designed a coding scheme that succeeds with a polynomially small failure probability. We revisit the question of conducting computations under this harsh type of noise and devise a computationally-efficient coding scheme that guarantees the success of the computation, except with an exponentially small probability. This higher degree of correctness matches the case of coding schemes with a bounded fraction of noise. Our simulation of an $N$-bit noise-free computation in the presence of $T$ corruptions, communicates an optimal number of $O(N+T)$ bits and succeeds with probability $1-2^{-\Omega(N)}$. We design this coding scheme by introducing an intermediary noise model, where an oblivious adversary can choose the locations of corruptions in a worst-case manner, but the effect of each corruption is random: the noise either flips the transmission with some probability or otherwise erases it. This randomized abstraction turns out to be instrumental in achieving an optimal coding scheme.

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 figures

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., Comment: 8 pages, 1 page reference, 3 figures, Conference Cris 2022

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., Comment: 7 pages, 7 figures

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., Comment: 15 pages, 4 figures, updated minimaized version, from earlier arxiv.org/abs/1808.10493v4; Volume 331, Frontier Research in Astrophysics, III (FRAPWS2018)

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., Comment: 15 pages, 12 figures

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., Comment: 16 pages, 4 figure , Questions and Discussion; new sections and new updated arguments

We 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., Comment: 15 pages, 9 figures; minor editorial correction; accepted in PoS MULTIFREQUENCY 2017

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 (GRB) signal. Here we consider the possibility that a Neutron Star (NS), merging in a NS-NS or NS-BH system might be (soon) observed in correlation with any LIGO-VIRGO Gravitational Waves detection. We analyze as an example the recent case of the short GRB 170817A observed by Fermi and Integral. The associated Optical transient OT source in NGC4993 imply 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 our. Therefore even soft GRB photons, more spread 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., Comment: 12 pages, 12 figures

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) and IceCube (as well as Deep Core, PINGU) neutrino detectors do offer a novel way to largest trace of solar Flare: their sudden anti-neutrino (or neutrino) flare made by proton scattering and pion decays via Delta resonance production. 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, GeV up to hundred GeV, energies. We show the expected rate of signals for the most powerful solar flare occurred in recent decades., Comment: 5 pages, 4 figures, ICRC 2017

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 versus 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 mondane prompt charmed atmospheric neutrino component may explain most of the IceCube puzzles. If this near future, 2017-2018, it does not shine tau neutrino signals somewhere (by tau airshowers in AUGER, TA, ASHRA or double bang in IceCube) there are a list of consequences to face. These missing correlations and in particular the tau signature absence force us to claim : No Tau? No neutrino Astronomy., Comment: 7 pages, 4 figures, ICRC 2017; additional minor misprint corrections

The Sun albedo of cosmic rays at GeVs energy has been discovered recently by FERMI satellite. They are traces of atmospheric CR hitting solar atmosphere and reflecting skimming gamma photons. Even if relevant for astrophysics, as being trace of atmospheric solar Cosmic Ray 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 TeV 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: PeVs secondaries may be shining on Earth atmosphere in lunar shadows in a surprising rich way. One or a few gamma air-shower event inside the Moon shadows may occur each year in near future CTA or LHAASO TeVs gamma array detector, assuming a non negligible astrophysical TeV up to hundred TeV neutrino component (respect to our terrestrial ruling atmospheric ones); these signals will open a new wonderful passepartout keyhole for neutrino been seen along the Moon. The lunar solid angle is small and the muon or tau expected rate is rare, but future largest tau radio array as GRAND one might well discover such neutrino imprint., Comment: 15 pages, 2 figures

The most distant AGN, within the allowed GZK cut-off radius, have been recently candidate by many authors as the best location for observed UHECR origination. Indeed, the apparent homogeneity and isotropy of recent UHECR signals seems to require a far cosmic isotropic and homogeneous scenario involving a proton UHECR courier: our galaxy or nearest local group or super galactic plane (ruled by Virgo cluster) are too much near and apparently too much anisotropic in disagreement with PAO and TA almost homogeneous sample data. However, the few and mild observed UHECR clustering, the North and South Hot Spots, are smeared in wide solid angles. Their consequent random walk flight from most far GZK UHECR sources, nearly at 100 Mpc, must be delayed (with respect to a straight AGN photon gamma flaring arrival trajectory) at least by a million years. During this time, the AGN jet blazing signal, its probable axis deflection (such as the helical jet in Mrk501), its miss alignment or even its almost certain exhaust activity may lead to a complete misleading correlation between present UHECR events and a much earlier active AGN ejection. UHECR maps maybe anyway related to galactic or nearest (Cen A, M82) AGN extragalactic UHECR sources shining in twin Hot Spot. Therefore we defend our (quite different) scenarios where UHECR are mostly made by lightest UHECR nuclei originated by nearby AGN sources, or few galactic sources, whose delayed signals reach us within few thousand years in the observed smeared sky areas., Comment: 13 pages, 10 figures, minor editorial corrections, in press, JPS Conference Proceedings Vol. 9 (published on April 6, 2016) JPS Conference Proceedings,Proceedings of International Symposium for Ultra-High Energy Cosmic Rays October 2016, (UHECR2016)

The last few years, 2013-2016, the high energy neutrino events in ICECUBE and the last rich UHECR maps by AUGER and TA were hopefully opening a new High Energy astronomy age. Unfortunately the foreseen correlation between neutrino with best gamma X sources has not (yet) been found. The most celebrated GRB gamma sources do not correlate to any neutrino events. The expected Local Group anisotropy in UHECR within the nuleon GZK cut off, has just fade away. UHECR events from Virgo are almost absent. Above two hundred TeV energy tau neutrino might shine by double bang in detectable way in ICECUBE. Within a dozen of events no tau neutrino arised (yet) in ICECUBE. Finally GRBs Fireball models calling since decades for HE neutrinos correlated imprint at TeVs energy are not (yet) found. So many absences are making a huge question mark: is there a new reading key?

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 figures

The shorter-than-Schwarzschild 3C 279 variability flare on June 2015 is very puzzling. Its nature cannot be due to any NS merging nor to a medium sized (hundred million solar mass) BH collapse. Our preliminary model is based on the long-life (a third of a year) merging of a medium size BH (hundred of solar mass) jet spiralling toward the largest AGN one, (billion solar mass), that is dragging by tidal torques the medium small size BH jet along the main AGN 3C 279 one. The tidal torque is aligning both jets toward Earth. The twin overlapping blazars may offer at once a long and a short scale variability consistent with the surprising Fermi discovers., Comment: 7 pages, 1 figure, PoS

Every GRB model where the progenitor is assumed to be a highly relativistic hadronic jet whose pions, muons and electron pair secondaries are feeding the gamma jets engine, necessarily (except for very fine-tuned cases) leads to a high average neutrino over photon radiant exposure (radiance), a ratio well above unity, though the present observed average IceCube neutrino radiance is at most comparable to the gamma in the GRB one. Therefore no hadronic GRB, fireball or hadronic thin precessing jet, escaping exploding star in tunneled or penetrarting beam, can fit the actual observations. A new model is shown here, based on a purely electronic progenitor jet, fed by neutrons (and relics) stripped from a neutron star (NS) by tidal forces of a black hole or NS companion, showering into a gamma jet. Such thin precessing spinning jets explain unsolved puzzles such as the existence of the X-ray precursor in many GRBs. The present pure electron jet model, disentangling gamma and (absent) neutrinos, explains naturally why there is no gamma GRB correlates with any simultaneous TeV IceCube astrophysical neutrinos. Rare unstable NS companion stages while feeding the jet may lead to an explosion simulating a SN event. Recent IceCube-160731A highest energy muon neutrino event with absent X-gamma traces confirms the present model expectations., Comment: 9 pages, 6 Figures

The Gravitational Wave (GW) events GW150914, GW151226, GW170104 detected by LIGO were a record of Black Hole binary merging system (BH-BH) very probably in nearly empty or a vacuum space; such a kind of events will be mostly with no baryon mass (plasma or dense masses) and therefore mute or blind in any correlated gamma band. If the GWs events might be born inside a globular cluster, a star forming region or along a spiral AGN accretion disk their additional accreting mass may be the needed baryon load to explode and shine: in those dense places. BH BH collapse may also offer an optical X and gamma afterglow via their baryon lightening and photon tracks. Only very nearby (tens Mpc) BH Neutron Star (NS) or NS NS cannibal merging might be guaranteed and associated also with a desired, visible and correlated spherical NS explosion (kilonova one); they require much lower threshold or just nearer distances. Indeed such a very exceptional GW170817 GRB170817a event occurred last August 2017; it took place and it was related to a very first NS NS collapse in a SN kilonova spherical explosion. The GRB170817a gamma, X, radio signature it was exceptional in many features . Its unique values (softer, weaker, the most near and long life one) made GRB170817a very possibly an off-axis jet detection. However there are solid arguments that suggest that such a GRB are not just blazing within a collimated beam jet but that they are also shining in a wider spread gamma equatorial disk blazing, orthogonal to the jet itself. In a few words we were observing the event not along its jet but mostly orthogonal to it. This GRB170817a geometry may better explain the otherwise unexpected beamed to us event. In this paper therefore we summarize the astrophysical and the cosmological signature of such a long desired multiple astronomy., Comment: 18 pages, 3 figures; updated text to recent data as GW 170817 and GRB 170817a

UHECR and UHE neutrino map correlation seem to most inconclusive. We show here that a few peculiar UHECR narrow clustering might be connected to a first UHE muon neutrino tracks. Moreover we discuss the best filtered and amplified UHE neutrino astronomy painted by up-going tau airshower. Their discover by new projects could be reached soon., Comment: 8 pages, 7 figure

We considered a novel energy storage system based on the compression of air through pumped water. Differently from CAES on trial, the proposed indirect compression leaves the opportunity to choose the kind of compression from adiabatic to isothermal. The energy storage process could be both fast or slow leading to different configuration and applications. These novel storage system are modular and could be applied in different scales for different locations and applications, being very flexible in charge and discharge process. The system may offer an ideal energy buffer for wind and solar storage with no (or negligible) environment hazard. The main features of this novel energy storage system will be showed together with overall energy and power data., Comment: 9 pages, 2 figures

High Energy Neutrino Astronomy has been revealed by a sudden change in the flavor composition around maximal energies since three years of recording in ice km detector. However these discover didn' t led to any clear promised Neutrino Astronomy land yet. No correlation with hard gamma sources was found. Moreover the astrophysical spectra expected at Fermi value, seem to converge to a softer value, also required to avoid any Glashow resonant neutrino signal. We suggest a main solution within a composite flux ruled by prompt atmospheric neutrinos. Nevertheless the recent discover of twentyone crossing muons at hundreds TeVs had shown a first narrow overlapped doublet and a correlated track with a peculiar hard UHECR event clustering pointing to a well known microjet in bynary precession; these first connections hint for a non negligible astrophysical component making neutrino astronomy anyway already more than a hope., Comment: 11 pages, 3 figures