Detecting Solar Neutrino Flare in Megaton and km3 detectors

Fargion, Daniele; Giacomo, Paola Di

doi:10.1016/j.nuclphysbps.2009.02.035

Cited by 7 publications

(16 citation statements)

References 5 publications

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“…To observe such an astronomy in the whole arrival direction (not just along the zenith but also in its azimuth) we suggest the doubling of the present Deep Core array strings, allowing a contemporaneous double string detection. The discovery of twenty GeV neutrino astronomy in Deep Core may find a bonus also in rare, but nearby and powerful, Solar Flare neutrino brightening [10] 4. Appendix: 3 flavor neutrino mixing The evolution equation for three neutrino mixing in matter reads :…”

Section: Discussionmentioning

confidence: 99%

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Foreseeing Neutrino spectra in Deep Core

Fargion

D’Armiento

Giacomo

et al. 2011

J. Phys.: Conf. Ser.

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Atmospheric muon neutrino in Deep Core (whose rate and spectra might be soon available) should exhibit an ′′ anomaly ′′ (due to tens GeV up-going muon neutrino suppression, converted into tau flavor) that must be imprinted in out-coming rate spectra. We estimate here our independent muon neutrino spectra based on SK and its projected record on Deep Core Channels. Our estimate (based on cosmic rays, muon records and tested Super-Kamiokande (SK) data) differs both in shape and in rate from other previous published spectra. The expected rate might exhibit a minimum near channel 6 of Deep Core strings and it should manifest strong signature for flavor mixing (mostly between channel 4-15) and a relevant ′′ anomaly ′′ for eventual CPT violation (MINOS like) written at channel 3-6, whose statistical weight (mainly at channel 5) might soon confirm or dismiss MINOS CPT claim [2]. At the flux minimum around channel 6, (a flux suppressed respect the non oscillated case at least by an order of magnitude) the atmospheric neutrino paucity offers a better windows to a twenty GeV Neutrino Astronomy. Therefore by doubling the string array we may foresee a richer rate and a more complete (zenith and azimuth) atmospheric neutrino distribution and an exciting first twenty GeV Astronomy.

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Section: Discussionmentioning

confidence: 99%

“…The role of neutrino muon and tau mixing among flavors has been observed since nearly 13 years and it has been foreseen already in different recent high energy astrophysical roles [1], [9], [10]. Recently MINOS results hint for a CPT violation in neutrino sector.…”

Section: Introductionmentioning

confidence: 99%

Foreseeing Neutrino spectra in Deep Core

Fargion

D’Armiento

Giacomo

et al. 2011

J. Phys.: Conf. Ser.

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“…Also consider a triplet along the galactic plane possibly related to Vela, the nearest and brightest gamma and radio source. see also [8]. and in particular see [9] FIGURE 3.…”

Section: Discussionmentioning

confidence: 99%

“…However the inner clustering centered on Cen A favor in my opinion, an unique source and a galactic field bending of UHECR. see [8], [9] UHECR far from a GZK volume may force us, surprisingly, to reconsider an exceptional model: Z-Shower one. Possibly connecting lowest neutrino particle (≃ 0.15 eV) mass with highest UHE (≃ 30ZeV)neutrino energies [5].…”

Section: Discussionmentioning

confidence: 99%

“…The consequences of the UHECR composition and source reflects into UHE (GZK [13] or cosmo-genic) neutrinos. The proton UHECR provide EeV neutrinos (muons and electron) whose flavor oscillation lead to tau neutrinos to be soon detectable [6] [2] 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 τ air-showers , or by Icecube km 3 neutrino fluorescence telescopes [6], [10], [8] [9] either by double bang [14], or long muon at few PeV energy. ZeV UHE neutrinos in Z-Shower model are possible source of horizontal Tau air-showers of maximal size and energy [6].…”

Section: Introductionmentioning

confidence: 99%

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UHECR Maps: mysteries and surprises

Fargion¹

2010

AIP Conference Proceedings

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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.Comment: 10 pages, 18 figure

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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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Detecting Solar Neutrino Flare in Megaton and km3 detectors

Cited by 7 publications

References 5 publications

Foreseeing Neutrino spectra in Deep Core

Foreseeing Neutrino spectra in Deep Core

UHECR Maps: mysteries and surprises

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

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