UHECR Maps: mysteries and surprises

Abstract. Ultra High Cosmic Rays made by He-like lightest nuclei might solve the AUGER extragalactic clustering along Cen A. Moreover He like UHECR nuclei cannot arrive from Virgo because the light nuclei fragility and opacity above a few Mpc, explaining the Virgo UHECR absence. UHECR signals are spreading along Cen A as observed because horizontal galactic arms magnetic fields, bending them on vertical angles. Cen A events by He-like nuclei are deflected as much as the observed clustered ones; proton will be more collimated while heavy (iron) nuclei are too much dispersed. Such a light nuclei UHECR component coexist with the other Auger heavy nuclei and with the Hires nucleon composition. We foresaw (2009) that UHECR He from Cen-A AGN being fragile should partially fragment into secondaries at tens EeV multiplet (D, H e 3 , p) nearly as the recent twin multiplet discovered ones (AUGER-ICRC-2011), at 20 EeV along Cen A UHECR clustering. Their narrow crowding occur by a posteriori very low probability, below 3 · 10 −5 . Remaining UHECR spread group may hint for correlations with other gamma (MeV − Al 26 radioactive) maps, mainly due to galactic SNR sources as Vela pulsar, the brightest, nearest GeV source. Other nearest galactic gamma sources show links with UHECR via TeV correlated maps. We suggest that UHECR are also heavy radioactive galactic nuclei as Ni 56 , Ni 57 and Co 57 ,Co 60 widely bent (tens degree up to ≥ 100 o ) by galactic fields. UHECR radioactivity (in and channels) and decay in flight at hundreds keV is boosted (by huge Lorentz factor Ni 10 9 − 10 8 ) leading to PeVs electrons and consequent synchrotron TeVs gamma offering UHECR-TeV correlated sky anisotropy. Moreover also rarest and non-atmospheric , and e neutrinos secondaries at PeVs, as the first two rarest shower just discovered in ICECUBE, maybe the first signature of such expected radioactive secondary tail.

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

Fargion¹,

D’Armiento²

2011

Preprint

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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. Indeed at first [1] UHECR did seem to follow the GZK cut off and to correlate with SGP, (even if a few of us disagreed [8],[14]). Recently [3] the last 69 UHECR did not longer follow the SGP map, opening the way to very different correlations [3], and extreme bending connection [18] ; we reconfirm here our Lightest Nuclei interpretation [8],[9],[10], [11], [12], 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.

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UHECR Maps: mysteries and surprises

Cited by 3 publications

References 14 publications

Is Cen A surrounded by tens-EeV UHECR multiplet?

Is Cen A surrounded by tens-EeV UHECR multiplet?

TeV gamma-UHECR anisotropy by decaying nuclei in flight: First neutrino traces?

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

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