Lightest Nuclei in UHECR versus Tau Neutrino Astronomy

Fargion, Daniele; D’Armiento, D.; Paggi, P.; Patrì, Stefano

doi:10.1016/j.nuclphysbps.2009.03.083

Cited by 15 publications

(29 citation statements)

References 15 publications

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“…This opportunity is appealing to some authors because a hundred Mpc distance radius guarantees enough sources and homogeneity [6,18]; see Fig.3, 4. However, the unique UHECR particles that may travel so far, as we mentioned are protons, while PAO models and simulation composition recently favor a mix of lightest nuclei (He) together with light ones (Be, B, C and N), as we did suggested, independently, since long time [16,17], due to the problematic Virgo absence and the observed smearing angles.…”

Section: Far Uhecr Bending Path In Random Walkmentioning

confidence: 73%

See 1 more Smart Citation

Uncorrelated Far Active Galactic Nuclei Flaring with Their Delayed Ultra High Energy Cosmic Rays Events

Fargion

Oliva

Lucentini

2018

Proceedings of 2016 International Conference on Ultra-High Energy Cosmic Rays (UHECR2016)

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The most distant Active Galactic Nuclei (AGN), within the allowed Greisen-Zatsepin-Kuzmin (GZK) cut-off radius (≲ 100 Mpc), have been recently candidate by many authors as the best location for the observed Ultra High Energy Cosmic Rays (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 the Virgo cluster) are too near and apparently too anisotropic to be in agreement with the (Pierre Auger Observatory (PAO) and Telescope Array (TA) almost-homogeneous data sample. However, the few and mild UHECR observed clustering, the so called North and South Hot Spots, are smeared in wide (±18 • ) 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 Mrk 501), 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 may be anyway related to galactic or nearest (Cen A, M82) AGN extragalactic UHECR sources shining in twin Hot Spot. Therefore we defend our (quite different) scenario where UHECR are mostly made by lightest UHECR nuclei originated by nearby AGN sources, or few galactic sources, whose delayed signals are reaching us within few thousand years in the observed smeared sky areas.

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Section: Far Uhecr Bending Path In Random Walkmentioning

confidence: 73%

“…One of course may wonder if this is not the same case of the nearest AGN, as we did suggested since 2008 [16], made by light and lightest nuclei [17]. In this case, indeed, the bending angle is scaling with the atomic number Z (Z He = 2, Z Li = 3, Z Be = 4, Z B = 6).…”

Section: Lightest Nuclei Uhecr and Their Time Delaymentioning

confidence: 76%

Uncorrelated Far Active Galactic Nuclei Flaring with Their Delayed Ultra High Energy Cosmic Rays Events

Fargion

Oliva

Lucentini

2018

Proceedings of 2016 International Conference on Ultra-High Energy Cosmic Rays (UHECR2016)

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“…We found that Cen A (the most active and nearby extragalactic AGN) is apparently the most shining UHECR source whose clustering (almost a quarter of the event) along a narrow solid angle (whose opening angular size is C171) [5] is convincing and in agreement with lightest nuclei [21,27,4]. However the main question is related to remaining majority of events.…”

Section: Overlapping G and Uhecr Mapsmentioning

confidence: 69%

“…The consequences of the UHECR composition and source distances should reflect, by interaction with relic photons, to UHE secondaries signals made by photo-pion production or photonuclear disruption as the well known GZK [2] or cosmo-genic neutrinos. The proton UHECR provide EeV neutrinos (muons and electron) whose flavor oscillation lead to tau neutrinos to be soon detectable [10,20] by upward tau air-showers; the UHECR lightest nuclei model provide only lower energy, tens PeV, neutrinos detectable in a very peculiar way by AUGER fluorescence telescopes or in ARGO array by horizontal t air-showers, or by Icecube km 3 neutrino telescopes [10,27,4] either by double bang [11], or by long muon at few PeV energy. Let us recall that ZeV UHE neutrinos in Z-Shower model are also possible source of horizontal Tau air-showers of maximal size and energy [10,9].…”

Section: A Two Decades Of Random Uhecr Puzzlesmentioning

confidence: 99%

TeV sky versus AUGER one: Are UHECR also radioactive, heavy galactic nuclei?

Fargion

2012

Nuclear Instruments and Methods in Physics Research Section A:

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UHECR (Ultra High Cosmic Rays) made by He-like lightest nuclei might solve the AUGER extragalactic clustering along Cen A: He UHECR cannot arrive from Virgo because the light nuclei fragility and opacity above few Mpc; UHECR signals are clustering along Cen-A spreading as observed by horizontal galactic arms magnetic fields, along random vertical angles. Cen A events by He-like spread along a width angle as large as the observed clustered one; such a light nuclei coexist with the Auger heavy nuclei and with the Hires nucleon composition. UHECR He being fragile should partially fragment in secondaries at tens EeV multiplet (D,He3,p) almost as it occurs in the very recent UHECR multiplet at 20 EeV along Cen A UHECR clustering. Their narrow crowding within a tiny (Cen A-centric disk) observation area (below 10−2 of the whole AUGER sky) aligned with Cen A may occur by a very low probability, below 3×10−5. Remaining UHECR spread group show correlations with other γ (MeV-Al26 radioactive) maps, mainly due to galactic SNR sources as Vela pulsar, the brightest, nearest GeV source. Other nearest galactic γ sources (as partially Crab and Galactic Center core) show links with UHECR via TeV correlated maps. We speculate here that UHECR are also heavy radioactive galactic nuclei as Ni56, Ni57 and Co57, Co60 widely bent (tens degree up to ≥100°) by galactic fields. UHECR radioactivity (in β and γ channels) and decay in flight at hundreds keV is boosted (by huge Lorentz factor ΓNi≃109−108) leading to TeVs γ correlated sky anisotropy. Tau neutrinos secondaries and their tau airshowers at horizons may rise (from hundreds TeVs–PeVs) in future ICECUBE, ANTARES double bang events, or in ARGO and ASHRA horizons or in AUGER or TA airshowers at PeVs–EeV energies, showing the expected Neutrino astronomy link to UHECR decay in flight

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“…However, the two earliest and main red colored UHECR Hot Spots were observed respectively by TA (2014-2016, North sky) and by Auger (2007-2018, South sky) are not correlated at all with the Virgo central direction. This remarkable Virgo absence is the Rosetta stone that forced us [19], a decade ago, toward the lightest [20] UHECR nuclei nature. Indeed we suggested the presence of a severe filter to stop the expected Virgo abundant UHECR events; if UHECR were protons the center of this map in the Fig.1 should shine brightly.…”

Section: The Virgo Absence and The Two Hot Spotsmentioning

confidence: 99%

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

Fargion¹,

Lucentini²,

Khlopov³

2018

Proceedings of XII Multifrequency Behaviour of High Energy Cosmic Sources Workshop — PoS(MULTIF2017)

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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.

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Lightest Nuclei in UHECR versus Tau Neutrino Astronomy

Cited by 15 publications

References 15 publications

Uncorrelated Far Active Galactic Nuclei Flaring with Their Delayed Ultra High Energy Cosmic Rays Events

Uncorrelated Far Active Galactic Nuclei Flaring with Their Delayed Ultra High Energy Cosmic Rays Events

TeV sky versus AUGER one: Are UHECR also radioactive, heavy galactic nuclei?

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

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