Radioactivity and fragmentation of UHECR: Correlating gamma anisotropy and neutrino PeV events

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 degree 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 (Ni,Co,Al,D, neutron) light and heavy UHECR nuclei in GRB-SGRs-jet, 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 TeV anisotropy, and also offering a very realistic source of first, otherwise puzzling, observed PeV neutrinos. Evidences for such relativistic Ni jet in 4U1630-47 system has been observed recently by D\'iaz Trigo collaboration.Comment: 6 pages, 5 figures: corrections following referee comments and suggestions. arXiv admin note: text overlap with arXiv:1207.0254, arXiv:1201.015

GRBs by thin persistent precessing lepton Jets: the long life GRB110328 and the Neutrino signal

Gamma Ray Burst sources are apparently evolving around us in a harder and brighter samples at far and far redshift. The average output may range from a near Supernova (nearest events) output to a billion time that power for most distant events. Such a tuned evolution around us is not an anti-copernican signature. It is a clear imprint of a off-axis (nearest sources) beaming versus a rarest in-axis blazing (far redshift sources) by a thin relativistic beam (Lorentz factor up ten thousand or above, corresponding to micro-nano steradian solid angle). The main consequence is the rarer and rarer presences of hardest gamma events (hundreds MeV, GeVs, tens GeVs), nearly one over a twenty, partially opaque by IR-gamma cut-off, observed with difficulty at largest redshift inside their thinner beamed jets. For this reason these rarest tens GeV beamed events, even observed by EGRET and Fermi, are hardly seen at hundred GeV by Cherenkov telescope (Magic,Hess,Veritas) on Earth. For the same reason and because tens GeV neutrino energy is below Icecube thresholds (threshold above hundreds GeV) we have not been observed yet a neutrino GRB. However if the GRBs primaries contains tens GeV neutrino traces (at comparable GRB gamma rate) their presence may rise in few years at Deep Core (a more dense array inside ICECUBE) detector whose lower threshold, ranges just one or few tens GeV energy. Moreover the very recent X ray persistent GRB110328, whose understanding was first associated to a cannibal star AGN eating, but now evolved to a cannibal AGN feeding beamed jet, it is, more naturally consistent to our thin jet GRB (by few solar mass compact source, not any AGN) spinning, precessing and blazing whose geometry is partially aligned and stable (than other GRBs) to us: its decay law and its average output is fully consistent with our earliest proposals.Comment: 7 pages, 5 figures, 1 table; http://sait.oat.ts.astro.it/MSAIt830112/PDF/2012MmSAI..83..312F.pd

UHECR besides CenA: hints of galactic sources

Ultra High Energy Cosmic Rays, UHECR, maybe protons, as most still believe and claim, or nuclei; in particular lightest nuclei as we advocated recently. The first (Auger Collaboration) nucleon proposal (2007)[2] foresaw to trace clearly the UHECR GZK Universe reaching far (up to 100 Mpc) Super-Galactic-Plane, with little angular dispersion. On the contrary Lightest Nuclei model (2008)[3], inspired by observed composition and by nearest CenA clustering (almost a quarter of the AUGER events) explains a modest and narrow (few Mpc) Universe view, as well as the puzzling Virgo absence: lightest nuclei offer a fragile (and therefore very nearby) blurred Astronomy. Here we address to a part of the remaining scattered events in the new up-dated Auger map (March 2009-ICRC09). We found within rarest clustering the surprising imprint of a few galactic sources, a partial component of UHECR sources. In particular we recognize a first trace of Vela, brightest gamma and radio galactic source, and smeared sources along Galactic Plane and Center. The clustering may imply additional tails of fragments (by nuclei photo-dissociation) at half energies. The UHECR light-nuclei fragility and opacity may also reflect into a train of secondaries as gamma and neutrinos UHE events at tens-hundred PeVs. These UHE neutrinos might be detectable in a coming future within nearest AUGER and Array Fluorescence Telescope views,(few km distances) by fast fluorescence flashing of horizontal up-going tau Air-showers.Comment: 3 pages, 6 figures + 1 original Map figure (from public web service SCINEGHE Oct. 2009: Daniele Martello for AUGER Collab: http://agenda.infn.it/conferenceOtherViews.py?view=standard&confId=1369, Talk n.21

Apart Cen A are UHECR mostly heavy radioactive and galactic nuclei?

Earliest AUGER UHECR anisotropy correlated with AGN within a GZK Universe almost fade away. Recent UHECR mass compositions did show a negligible nucleon composition and an UHECR nuclei (light or heavy) signature. The absence of UHECR events toward the Virgo cluster, an unique spread clustering of events around Cen-A, our nearest AGN, suggested a He-like nuclei as the main extragalactic UHECR component from Cen A, coexisting with Auger and HIRES composition. Because the light nuclei fragility such He UHECR cannot arrive from Virgo. Multiplet at twenty EeV along Cen A recently discovered by Auger confirm this interpretation to be indebt to fragments (D;He3; p) that had to reach us along the same UHECR. Remaining majority of UHECR clustering are partially correlated with a gamma noise at (1-3 MeV) in Comptel sky, linked to Al 26 galactic radioactive map as well as to a few TeV gamma anisotropy maps; rare UHECR triplet are overlapping on Vela TeV anisotropy. Therefore UHECR might be also (or mostly) heavy radioactive galactic nuclei as Ni55, Ni56, Ni57 and Co57 bent from the sources whose gamma and beta radioactivity and decay in flight is boosted (by Lorentz factor near a billion), leading to TeV correlated sky anisotropy. Galactic UHECR signals inside the inner center maybe suppressed by Lorentz bending forces. More clustering around external galactic plane is expected. Magellanic Cloud and Magellanic Stream may also rise in UHECR maps (as well as in multiplet). Future UHECR clustering might be observed around Cas A and Cygnus by T.A. The UHECR spectra cut off may be just the imprint of a galactic confinement and-or a spectroscopic heavy composition decrease step.Comment: 5 pages, 3 figures, few corrections following referee comment

GRBs, Fireballs and Precessing Gamma Jets

Fireballs are huge isotropic explosions models widely believed to explain Gamma Ray Burst, GRBs (Piran,1999); ever-new versions consider wide beamed (10^o) Jet explosions hitting external shells. On the contrary, since 1994-1998, we argued (Fargion 1995-2000; see also Blackman et all.1996) that GRBs (as well as Soft Gamma Repeaters SGR) are spinning and precessing Gamma Jets, produced by collimated e^+,e^- Jet via Inverse Compton Scattering, in a very narrow (0.1^o) angles, blazing and flashing the observer. The Jet arises in Super-Nova (SN) explosions; its energy decays slowly from earliest SN powers (corresponding to GRB) toward lower stable power as Soft Gamma Repeaters (SGR) regimes. GRBs and SGRs shared (sometimes) same spectra and time structure: then SGRs are low-power GRBs, but without SN relics (or GRB afterglows, signatures of Jets in SN-GRBs). Moreover weak isolated X-ray precursor signals,(such as GRB980519, GRB981226,GRB000131), corresponding to huge isotropic, sim 10^{47} erg s^{-1}, followed by the extreme GRB, sim {10^{52}} erg s^{-1} powers, disagree with any Fireball explosive scenarios. We naturally interpret these X-Ray precursors as rare earliest marginal blazes of outlying X conical precessing Jet tails, surrounding the gamma Jet, later hitting in-axis as a GRB.Comment: 3 pages, LaTeX,10 PS figures, to appear in Procs. of the 2nd Workshop "Gamma-Ray Bursts in the Afterglow Era",Rome,Oct.17-20,200

GRBs and SGRs as precessing gamma jets

The GRB980425-SN1998bw association put in severe strain and contradiction the simplest "candle" fireball model for GRBs. We probed that statistically the association is reliable, the energy luminosity and probability puzzles between cosmic and near by GRBs find a solution within a precessing gamma jet model either for GRBs and SGRs. The expected repetitivity for GRB 980425 has been already, probably, observed on GRB980712.Comment: 18 pages, Late

Detecting Solar Neutrino Flare in Megaton and km^3 detectors

To foresee a solar flare neutrino signal we infer its upper and lower bound. The upper bound was derived since a few years by general energy equipartition arguments on observed solar particle flare. The lower bound, the most compelling one for any guarantee neutrino signal, is derived by most recent records of hard Gamma bump due to solar flare on January 2005 (by neutral pion decay).The observed gamma flux reflects into a corresponding one for the neutrinos, almost one to one. Therefore we obtain minimal bounds already at the edge of present but quite within near future Megaton neutrino detectors. Such detectors are considered mostly to reveal cosmic supernova background or rare Local Group (few Mpc) Supernovas events. However Megaton or even inner ten Megaton Ice Cube detector at ten GeV threshold may also reveal traces of solar neutrino in hardest energy of solar flares. Icecube, marginally, too. Solar neutrino flavors may shine light on neutrino mixing angles.Comment: 4 pages,4 figure