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D. Fargion

Publications and source records attributed to D. Fargion.

At least 19 recordsLinked to original sources

PeV neutrons as origin of separated SS433 TeV signals

The SS433, a well-known binary system with an internal black hole, have shown since half a century, an inner (a few year light distances) twin precessing jets spirals. These beams are made by tidal forces while stripping mass from large stellar companion feeding an inner BH accretion disk and an orthogonal accelerating twin jet. From it, the radio, X gamma jet emission. A couple of years ago H.E.S.S telescope as well as HAWC and LHAASO array detectors, discovered also the surprising signature of an unexpected far twin separated gamma beam at tens TeV energy. At a hundred light years distances from its central source. We suggest that it is the legacy of a past rare eruption, a century ago, of tens PeV (10^16 eV) relativistic twin neutron beams. Their beta decay in flight at far distances, into proton, neutrino and in particular into tens TeV electrons, could feed the observed TeV gamma traces. They are originated by the same secondary tens TeV electrons emitting hard gamma, by Inverse Compton Scattering onto interstellar infrared photons.

astro-ph.HE

Paucity of downward UHE neutrino tracks in IceCube versus unexpected huge KM3-230213A event: solving the puzzles?

Recently the ARCA array detector published the down-ward-horizontal event: the KM3-230213A. It appeared as the most energetic neutrino ever observed: about 200 PeV (2 10^17 eV) up to EeV (10^18 eV) energy. This huge value, is puzzling. It is not statistically consistent with several upper bound derived by two greater and longer life detectors: by IceCube and in particular by AUGER array. Asymmetry in recent IceCube neutrino alert tracks upward and downward at same horizontal angles as ARCA one, suggest that they are mostly polluted atmospheric muon bundles. This paucity also disfavor the skimming neutrino interpretation by ARCA. We suggest that the array floating and bending in the deep sea may lead, sometime, to a misleading geometry that is pointing to a wrong arrival angle direction: a much less horizontal muon (neutrino) track respect to a much real one, more inclined and vertical, due to atmospheric muon bundle or charmed single event. Contrary to present argument, if such a rare event would be soon rediscovered in data or re-observed, it would open the road to a new guaranteed Tau neutrino Astronomy. At EeV energy such upward tau air-showers should shine AUGER telescopes or blaze future satellite in Space. A previous model in astrophysics considered energetic neutrino E>>100 EeV, neutrino scattering, onto cosmic, relic, light mass ones. Their ultra-relativistic Z boson resonance formation and its decay in flight would produce hadron UHECR relics around tens-hundred EeV energy. Explaining how sources located at far distances, above the usual GZK hundred Mpc, cut off ones, may shine and cluster in AUGER or TA data.

astro-ph.HE

SS433 Microquasar Jet and the TeV Resurgence beam

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.

astro-ph.HE

How can we explain last UHERC anisotropies?

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.

astro-ph.HE

A charming ICECUBE discover?

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.

astro-ph.HE

No guaranteed neutrino astronomy without (enough) double bang tau and downward HESE muon tracks: An update version

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.

astro-ph.HE

Uncorrelated far AGN flaring with their delayed UHECRs events

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.

astro-ph.HE

2013-2016 review: HE Neutrino and UHECR Astronomy?

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?

astro-ph.HE

Why not any tau double bang in Icecube, yet?

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.

astro-ph.HE

Crossing muons in Icecube at highest energy: Cornerstone to neutrino astronomy

Highest energy neutrino events (contained) in cubic km ICECUBE detector resulted in last three years to be as many as $37-2=35$ signals (two of those having been recently discharged); these tens-hundred TeV (32 energetic events) up to rarest (only 3) PeV cascade showers, proved to have an extraterrestrial origin. The UHE neutrino flavor transition from a $ν_μ$ atmospheric dominance (over $ν_{e}$ showers at TeV energy), toward a higher energy shower cascade ($ν_{e}$, $ν_τ$) events at few tens TeV up to PeV energy is a hint of such a fast extraterrestrial injection. The majority (28 out of 35) of all these events are spherical cascade; their consequent smeared map is inconclusive. The additional rarest $9-2=7$ muon tracks, while being sharp in arrival directions, did not offer any correlated clustering nor any overlapping within known sources. We recently suggested that the highest energy (tens-TeV) crossing muon along the ICECUBE, mostly at horizons or upcoming, are the ideal tool able to reveal soon such clustering or even any narrow angle pointing to known (IR, X, Radio or $γ$) sources or self-correlation in rare doublet or triplet: a last hope for a meaningful and short-time $ν$ Astronomy. Any crossing muons clustering along galactic sources or within UHECR arrivals might also probe rarest UHECR event made by nuclei or neutrons. Within three years of ICECUBE data all the non-contained crossing highest energy muons above few tens TeV may be several dozens, possibly around $54$ (27 for upward ones), mostly enhanced along horizontal edges, painting known sources and/or self-correlating in doublets or rarest triplet (if steady or transient nearby source are at sight). Recent preliminary ICECUBE presentation on crossing muons are consistent with present preliminary muon rate estimate.

astro-ph.HE

Neutrino oscillations along the Earth to probe flavor parameters: a NeuWorld

On 2010 MINOS experiment was showing an hint of possible different mass splitting and mixing angles for neutrinos and anti-neutrinos, suggesting a charge-parity-time (CPT) violation in the lepton sector; last year 2012 a second result from MINOS showed a reduced discrepancy between the two set of parameters, nearly compatible with no CPT violation. We proposed an experiment for more precise estimation of neutrino oscillation parameters being useful not only for a complete discrimination for CPT scenarios, but also for mass hierarchy and theta 13 determination, and mostly for the first oscillated detection of tau and antitau neutrinos. We show an experiment, (the longest baseline neutrino oscillation test available by crossing most of Earth diameter, a NeuWorld), that may improve the oscillation measurement and disentangle at best any hypothetical CPT violation while testing tau appearance at the same time of the muon disappearance correlated. The experiment use a neutrino beam crossing the Earth, within an OPERA-like experiment from CERN (or Fermilab), in the direction of the IceCube DeepCore detector at the South Pole. Such a tuned beaming and its detection may lead to a strong signature of neutrino muon-tau mixing (nearly one anti tau or two tau a day, with 10 sigma in a year), even for an one per-cent OPERA-like NeuWorld experiment.

hep-ph

UHECR bending, clustering and decaying feeding gamma anisotropy

Ultra High Cosmic Rays) made by He-like lightest nuclei might fit clustering along Cen A. Moreover He like UHECR nuclei explain Virgo absence because the light nuclei fragility and opacity above a few Mpc. We foresaw (2009) that UHECR He from Cen-A AGN being fragile should partially fragment into secondaries at tens EeV multiplet (D,He^{3},p) as the recent twin multiplet discovered ones (AUGER-ICRC-2011), at 20 EeV along Cen A UHECR clustering. We suggest that UHECR are also heavy radioactive galactic nuclei as Ni^{56}, Ni^{57} and Co^{57} widely bent (tens degree up to 100 degrees) by galactic fields. UHECR radioactivity and decay in flight at hundreds keV is boosted (by huge Lorentz factor (billion) leading to PeVs electrons and consequent synchrotron TeVs gamma offering UHECR-TeV correlated sky anisotropy. Electron and tau neutrinos secondaries at PeVs maybe the first signature of such expected radioactive secondary tail.

astro-ph.HE

Inconsistence of super-luminal Cern-Opera neutrino speed with observed SN1987A burst and neutrino mixing for any imaginary neutrino mass

We tried to fit in any way the recent Opera-Cern claims of a neutrino super-luminal speed with observed Supernova SN1987A neutrino burst and all (or most) neutrino flavor oscillation. We considered three main frame-works: (1) A tachyon imaginary neutrino mass, whose timing is nevertheless in conflict with observed IMB-Kamiokande SN1987A burst by thousands of billion times longer. (2) An ad hoc anti-tachyon model whose timing shrinkage may accommodate SN1987A burst but greatly disagree with energy independent Cern-Opera super-luminal speed. (3) A split neutrino flavor speed (among a common real mass relativistic neutrino electron component and a super-luminal neutrino μ) in an ad hoc frozen speed scenario that is leading to the prompt neutrino de-coherence and the rapid flavor mixing (between electron and muon ones) that are in conflict with most oscillation records. Therefore we concluded that an error must be hidden in Opera-Cern time calibration (as indeed recent rumors seem to confirm). We are also reminding the relevance of the guaranteed minimal atmospheric neutrino mass whose detection may be achieved by a milliseconds graviton-neutrino split time delay among gravity burst and neutronization neutrino peak in any future SN explosion in Andromeda recordable in Megaton neutrino detector.

astro-ph.HE

Cen A persistence and Virgo absence versus updated maps to understand UHECR nature

Ultra High Cosmic Rays (UHECR) should be tracing their sources, making a new astronomy. Their events counting are finally growing, by Auger experiment, into cosmic sky. Their map should follow the mass distribution in a narrow cosmic volume (the GZK cut off region, correlated with Super Galactic Plane (SPG) or Local Group) if they were protons, as most expected. Recently the last 69 UHECR did not longer follow the SGP map, opening the way to very different correlations, and extreme bending connection; we reconfirm here our Lightest Nuclei interpretation, while showing here the last event over different radio, X, Gamma and tens TeV CR maps. The Virgo Cluster absence, the persistence of UHECR clustering along Cen A, the first triplet along Vela seem to confirm light nuclei UHECR understanding, implying a very narrow Universe view, even partially of galactic origin. UHECR fragments might follow (at half, fourth of the energy) the same UHECR map with a tail or a crown clustering around main UHECR group. Also secondary gamma and UHE neutrino might trace partially those maps. Tau neutrinos at EeV or PeVs may play a role in correlating UHECR map and disentangling nucleon from nuclei nature, possibly in Auger Fluorescence Telescopes, by night horizontal up-going tau airshowers.

astro-ph.HE

Deep Core muon neutrino rate and anisotropy by mixing and CPT violation

Neutrinos are allowed to mix and to oscillate among their flavor. Muon and tau in particular oscillate at largest values.Last Minos experiment claimed possible difference among their matter and anti-matter masses, leading to a first violation of the most believed CPT symmetry.Isotropically born atmospheric muon neutrino at 20-80 GeV, while up-going, they might be partially suppressed by mixing in analogy to historical SuperKamiokande muon neutrino disappearance into tau, leading to large scale anisotropy signals. Here we show an independent muon rate foreseen in Deep Core based on observed SK signals extrapolated to DeepCore mass and its surrounding. Our rate prediction partially differ from previous ones. The neutrino muon disappearance into tau is leading to an anisotropy in vertical up-going muon track: in particular along channel 3-5 we expect a huge rate (tens of thousand of events) of neutral current events, charged current electron and inclined crossing muons. Moreover at channel 6-9 we expect a severe suppression of the rate due to muon disappearance (in CPT conserved frame). Such an anisotropy might be partially tested by more than one string detection at E> 45 GeV energy. A CPT violation may induce a more remarkable suppression of vertical up-going tracks because of larger anti-neutrino muon reduction for E> 35 GeV.

astro-ph.HE

Characterizing Complex Particle Morphologies Through Shape Matching: Descriptors, Applications, and Algorithms

Many standard structural quantities, such as order parameters and correlation functions, exist for common condensed matter systems, such as spherical and rod-like particles. However, these structural quantities are often insufficient for characterizing the unique and highly complex structures often encountered in the emerging field of nano and microscale self-assembly, or other disciplines involving complex structures such as computational biology. Computer science algorithms known as "shape matching" methods pose a unique solution to this problem by providing robust metrics for quantifying the similarity between pairs of arbitrarily complex structures. This pairwise matching operation, either implicitly or explicitly, lies at the heart of most standard structural characterization schemes for particle systems. By substituting more robust "shape descriptors" into these schemes we extend their applicability to structures formed from more complex building blocks. Here, we describe several structural characterization schemes and shape descriptors that can be used to obtain various types of structural information about particle systems. We demonstrate the application of shape matching algorithms to a variety of example problems, for topics including local and global structure identification and classification, automated phase diagram mapping, and the construction of spatial and temporal correlation functions. The methods are applicable to a wide range of systems, both simulated and experimental, provided particle positions are known or can be accurately imaged.

cond-mat.soft

UHECR Maps: mysteries and surprises

The rise of nucleon UHECR above GZK astronomy made by protons is puzzled by three main mysteries: an unexpected nearby Virgo UHECR suppression, a rich crowded clustering frozen vertically (north-south) along Cen A, a composition suggesting nuclei and not nucleons. The UHECR map, initially consistent with GZK volumes, to day seem to be not much correlated with expected Super Galactic Plane. Moreover slant depth data of UHECR from AUGER airshower shape do not favor the proton but points to a nuclei, while HIRES, on the contrary favors mostly nucleons. We tried to solve the contradictions assuming UHECR as light nuclei (mostly He) spread by planar galactic fields, randomly at vertical axis. The He fragility and its mass and charge explains the Virgo absence (due to opacity above few Mpc) and the Cen A spread clustering (a quarter of the whole sample). However more events and rare doublets and clustering elsewhere are waiting for an answer. Here we foresee hint of new UHECR component: galactic ones. Moreover a careful updated views of UHECR sky over different (Radio,IR,Optics, X,gamma, TeV) background are also favoring forgotten revolutionary Z-shower model. Both Z-Shower, proton GZK and Lightest nuclei UHECR models have dramatic influence on expected UHE neutrino Astronomy: to be soon revealed by UHE tau neutrino induced air-showers in different ways.

astro-ph.HE

Coherent and random UHECR Spectroscopy of Lightest Nuclei along CenA: Shadows on GZK Tau Neutrinos spread in a near sky and time

Earliest 2007 UHECR anisotropy findings and ICRC AUGER updated maps and clustering confirms our understanding of CenA as the main nearby UHECR source. Those events are mostly lightest nuclei, as He. The events are spread by galactic fields. We argue that the main UHECR event bending, along CenA, is spreading vertically (respect to horizontal spiral galactic fields) by random (and a final coherent) Lorentz force. The He-nuclei dominance is also well probed by detailed AUGER composition data. The Lightest nuclei are still compatible with most recent Hires composition results. Such lightest UHECR nuclei are fragile and opaque even to nearest Universe. Offering a very narrow local (ten Mpc) view. This opacity explain the otherwise puzzling Virgo persistent absence. The He photo-disruption in flight should lead to halves energy tail clustering (along the same CenA group), events made by deuterium, He3 and protons (or unstable neutrons). This tail anisotropy should be revaled. The consequent foreseen UHE neutrino by UHECR Lightest nuclei dissociation, at tens-a hundred PeV, may rise soon in AUGER and TA telescopes. Such neutrino signal are quite inclined upward fluorescent Tau air-showers at nearest (2 - 4 km) horizons, at middle-low telescope view zenith angles. Their air-showers will be opening and extending in widest azimuth angle and fastest angular velocity spread. Contrary to far EeV tau expected by popular GZK neutrinos. Even hard to observe these Tau Air-showers at tens and hundred PeVs may soon shine (in a peculiar way) at near telescope views and within a short (years) time, both in AUGER, HEAT and TA sky.

astro-ph.HE