Is Cen A surrounded by tens-EeV UHECR multiplet?

Fargion, Daniele

doi:10.1016/j.ppnp.2012.01.030

Cited by 5 publications

(11 citation statements)

References 20 publications

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“…Moreover the same twin tail of the events is aligned almost exactly ±0.1 rad along the UHECR train of events toward Cen A. Therefore the UHECR multiplet alignment at twenty EeV has an a priori probability as low as P (3, 2) ≃ 3 · 10 −5 of following the foreseen signature [11]. The incoherent random angle bending (2) along the galactic plane and arms, δ rm , while crossing along the whole Galactic disk L ≃ 20 · kpc in different (alternating) spiral arm fields and within a characteristic coherent length l c ≃ 2 · kpc for He nuclei is δ rm−He ≃…”

Section: Bending For He Uhecr and Fragments At 20 Eev Along Cen Amentioning

confidence: 83%

“…1). However, the crowding of the two train multiplet tail centers inside a very narrow disk area focused about the rarest Cen A UHECR source is remarkable, [11]. If UHECR are made by protons (as some AUGER and TA author believe), they will not naturally explain such a tail structure because these events do not cluster more than a few degrees, unlike the observed UHECR and the associated multiplet.…”

Section: Bending For He Uhecr and Fragments At 20 Eev Along Cen Amentioning

confidence: 94%

“…Our He-like UHECR fit the AUGER as well as the HIRES and TA composition traces. The He secondaries split in half (or a fourth) energy fragments along the Cen A tail the presence of which has being foreseen, published (and ignored) many times in recent years [24], [11]. Indeed, the dotted circle around Cen A containing two (of three) multiplets has a radius as small as 7.5 o extending in an area that is as small as 200 square degrees, below or near 1% of the AUGER observation sky.…”

Section: Bending For He Uhecr and Fragments At 20 Eev Along Cen Amentioning

confidence: 99%

“…It should be noted that the present anisotropy above GZK [6] energy 5.5 · 10 19 eV (if extragalactic) might leave a tail of signals: indeed the photo disruption of He into deuterium, tritium, He 3 and protons (and unstable neutrons), arising as clustered events at a half or a quarter (for the last most stable proton fragment) of the energy: protons being with a quarter of the energy but a half of the charge of the He parent may form a tail smeared around Cen-A at a twice larger angle [11]. We suggested looking for correlated tails of events, possibly in strings at low ≃ 1.5 − 3 · 10 19 eV along the Cen A train of events.…”

Section: Bending For He Uhecr and Fragments At 20 Eev Along Cen Amentioning

confidence: 99%

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Radioactive Uhecr Astronomy: Correlating Gamma Anisotropy and Neutrino Pev Events

Fargion

2013

Acta Polytech

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UHECR (Ultra High Energy Cosmic Rays) were expected to be protons, to fly straight and to suffer from a GZK (opacity on CMB radiation) cut off. AUGER suggested in 2007 that such early UHECR anisotropy was compatible with the foreseen Super-Galactic plane, while both HIRES and AUGER confirmed this apparent GZK cut-off in the spectra. However, the same AUGER composition since 2007 had favored nuclei (and not nucleons). The recent absence of narrow angle clustering in UHECR maps, as it should be expected for protons, the missing of events along the nearest Cluster Virgo, the wide spread (nearly 16 o angle) of UHECR along Cen A are in disagreement with the first proton-UHECR AUGER understanding. Since 2008 we had claimed a light nuclei role for the Cen A crowded area. However the ICECUBE absence of TeV neutrino clustering or anisotropy, its spectra steepening favors mostly a ruling atmospheric neutrino noise up to tens TeV. However two recent PeV neutrino event, cannot easily coexist or been extrapolated with such an atmospheric ruling scenario, or with GZK (either nucleons or nuclei) secondary expected spectra. Finally tens of TeV gamma anisotropy in ARGO-MILAGRO-ICECUBE maps may hardly be associated with known hadronic sources. We imagine such anisotropy ruled by diffused gamma secondaries, shining along UHECR bending and flight: radioactive light and heavy UHECR nuclei, while scattering or decaying in flight, may paint in the sky (by gamma, electrons and neutrinos secondaries) their trajectories and bending, connecting UHECR spread events with γ TeV anisotropy, and also offering a very realistic source of first, otherwise puzzling, observed PeV neutrinos.

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Section: Bending For He Uhecr and Fragments At 20 Eev Along Cen Amentioning

confidence: 83%

Section: Bending For He Uhecr and Fragments At 20 Eev Along Cen Amentioning

confidence: 94%

Section: Bending For He Uhecr and Fragments At 20 Eev Along Cen Amentioning

confidence: 99%

Section: Bending For He Uhecr and Fragments At 20 Eev Along Cen Amentioning

confidence: 99%

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Radioactive Uhecr Astronomy: Correlating Gamma Anisotropy and Neutrino Pev Events

Fargion

2013

Acta Polytech

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“…However in other more recent studies the correlations (as the North or South HOT SPOTS) has not been confirmed [11]. The 55 EeV UHECR (as well their EeV traces) being fragmented and decayed in flight may also shine secondaries in tens EeV energy range, as it has been foreseen and later observed around Cen-A twin train of events [17]; the same fragments being UHECR and possibly radioactive they might decay and shine in hundred TeV-PeVs energy too, making the observed TeVs anisotropy explained [1]. Therefore there is a good reason to try to overlap UHECR and neutrino signals, both the showering but mainly the muon tracks.…”

Section: The Uhecr Versus Uhe-neutrino Mapsmentioning

confidence: 91%

Why not any tau double bang in IceCube, yet?

Fargion¹,

Oliva²,

Ucci³

2016

Proceedings of Frontier Research in Astrophysics — PoS(FRAPWS2014)

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High Energy Neutrino Astronomy has been revealed by a sudden change in the flavor composition above 30 TeV since 2013 by IceCube detector: the fast growth of spherical showers over atmospheric muon track signal in IceCube marked the revolution. However these discover didn't led to the promised Neutrino-Astronomy-Land yet. AGN flaring are not correlated with these high energy tens TeV-PeV events. Brightest persistent or pulsed galactic sources are missing while no point source arise in the lower energy sky. GRB events do not correlate within any minute-hour lapse time windows along any neutrino event. Moreover the astrophysical hard spectra whose exponent was expected at Fermi value of −2, seem to converge from −2.2 to a softer −2.7 or −3.0 value, also needed to avoid unobserved Glashow resonant neutrino at 6.3 PeV energy. Finally a key question arises: why within the ten UHE neutrino, those harder than 200 TeV events (whose timing structure would allow IceCube to disentangle any double tau neutrino imprint) don't double bang anyway? We suggest a main solution within a composite flux mostly ruled by prompt atmospheric neutrinos. Nevertheless in the very recent discover of 21 through-going (crossing) muons at hundreds TeVs, whose tracks are more aligned and telling, is shown a first narrow doublet (and some of correlated UHECR clustered source); this points -or give hintsfor a non-negligible 10 − 20% astrophysical component, making neutrino astronomy already alive anyway.

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