2,014 research outputs found
Updated Z-Burst Neutrinos at Horizons
Recent homogeneous and isotropic maps of UHECR, suggest an isotropic cosmic
origin almost uncorrelated to nearby Local Universe prescribed by GZK (tens
Mpc) cut-off. Z-Burst model based on UHE neutrino resonant scattering on light
relic ones in nearby Hot neutrino Dark Halo, may overcome the absence of such a
local imprint and explain the recent correlation with BL Lac at distances of a
few hundred Mpc. Z-Burst multiple imprint, due to very possible lightest
non-degenerated neutrino masses, may inject energy and modulate UHECR ZeV edge
spectra. The Z-burst (and GZK) ultra high energy neutrinos (ZeV and EeV band)
may also shine, by UHE neutrinos mass state mixing, and rise in corresponding
UHE Tau neutrino flavor, whose charged current tau production and its decay in
flight, maybe the source of UHE showering on Earth. The Radius and the
atmosphere size of our planet constrains the tau maximal distance and energy to
make a shower. These terrestrial tau energies are near GZK energy limit. Higher
distances and energies are available in bigger planets; eventual solar
atmosphere horizons may amplify the UHE tau flight allowing tau showering at
ZeV energies offering a novel way to reveal the expected Z-Burst extreme
neutrino fluxes.Comment: 6 Pages, 9 figure
Cherenkov Flashes and Fluorescence Flares on Telescopes: New lights on UHECR Spectroscopy while unveiling Neutrinos Astronomy
Cherenkov Telescopes (as Magic, Hess and Veritas), while pointing
horizontally should reveal also the fluorescence flare tails of nearby
down-going air-showers. Such air-showers, born at higher (tens km) altitudes,
are growing and extending up to lowest atmospheres (EeVs) or up to higher (few
km) quotas (PeVs). Viceversa, as it has been foreseen and only recently
observed, the opposite takes place. Fluorescence Telescopes made for UHECR
detection may be blazed by inclined Cherenkov lights. The geomagnetic splitting
may tag the energy as well as the inclined shower footprint as seen in a recent
peculiar event in AUGER. Additional stereoscopic detection may define the event
origination distance and its consequent primary composition, extending our
understanding on UHECR composition, while unveling a novel tau Neutrino
Astronomy.Comment: 5 pages, 5 figures, Preprint submitted to Nuclear Instruments and
Methods A. Only editorial format chang
Air-Shower Spectroscopy at horizons
Horizontal and Upward air-showers are suppressed by deep atmosphere opacity
and by the Earth shadows. In such noise-free horizontal and upward directions
rare Ultra High Cosmic rays and rarer neutrino induced air-showers may shine,
mostly mediated by resonant PeVs interactions in air or by higher energy Tau
Air-showers originated by neutrino tau skimming the Earth. At high altitude
(mountains, planes, balloons) the air density is so rarefied that nearly all
common air-showers might be observed at their maximal growth at a tuned
altitude and directions. The arrival angle samples different distances and the
corresponding most probable primary cosmic ray energy. The larger and larger
distances (between observer and C.R. interaction) make wider and wider the
shower area and it enlarge the probability to be observed (up to three order of
magnitude more than vertical showers); the observation of a maximal
electromagnetic shower development may amplify the signal by two-three order of
magnitude (respect suppressed shower at sea level); the peculiar altitude-angle
range may disentangle at best the primary cosmic ray energy and composition.
Even from existing mountain observatory the up-going air-showers may trace,
above the horizons, PeV-EeV high energy cosmic rays and, below the horizons,
PeV-EeV neutrino astronomy: their early signals may be captured in already
existing gamma telescopes as Magic at Canarie, while facing the Earth edges
during (useless) cloudy nights.Comment: 9 pages, 9 figures, submitted to Prog. Part. Nucl. Phy
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
Galactic Gamma Halo by Heavy Neutrino annihilations?
The diffused gamma halo around our Galaxy recently discovered by EGRET could
be produced by annihilations of relic neutrinos N (of fourth generation), whose
mass is within a narrow range (Mz /2 < M < Mz). Neutrino annihilations in the
halo may lead to either ultrarelativistic electron pairs whose inverse Compton
Scattering on infrared or optical galactic photons could be the source of the
observed GeV gamma rays, or to prompt 100 MeV- 1 GeV photons (due to neutral
pion secondaries) born by N - anti N --> Z--> quark pairs reactions. The
consequent gamma flux (10 ^(-7)- 10^(-6) cm ^(-2) s^(-1) sr^(-1)) is well
comparable to the EGRET observed one and it is also compatible with the narrow
window of neutrino mass : 45 GeV < M < 50 GeV recently required to explain the
underground DAMA signals. The presence of heavy neutrinos of fourth generation
do not contribute much to solve the dark matter problem of the Universe, but it
may be easily detectable by outcoming LEP II data.Comment: 16 pages, Latex text,in press in Astroparticle Physics 199
TeV gamma-UHECR anisotropy by decaying nuclei in flight: first neutrino traces?
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. 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^{60}
widely bent by galactic fields. UHECR radioactivity (in and
channels) and decay in flight at hundreds keV is boosted (by huge Lorentz
factor (nearly a billion) leading to PeVs electrons and consequent synchrotron
TeVs gamma offering UHECR-TeV correlated sky anisotropy. Moreover also rarest
and non-atmospheric electron and tau neutrinos secondaries at PeVs, as the
first two rarest shower just discovered in ICECUBE, maybe the first signature
of such expected radioactive secondary tail.Comment: 7 pages,3 figures. arXiv admin note: substantial text overlap with
arXiv:1201.015
Splitting neutrino masses and showering into Sky
Neutrino masses might be as light as a few time the atmospheric neutrino mass
splitting. High Energy ZeV cosmic neutrinos (in Z-Showering model) might hit
relic ones at each mass in different resonance energies in our nearby Universe.
This non-degenerated density and energy must split UHE Z-boson secondaries (in
Z-Burst model) leading to multi injection of UHECR nucleons within future
extreme AUGER energy. Secondaries of Z-Burst as neutral gamma, below a few tens
EeV are better surviving local GZK cut-off and they might explain recent Hires
BL-Lac UHECR correlations at small angles. A different high energy resonance
must lead to Glashow's anti-neutrino showers while hitting electrons in matter.
In air, Glashow's anti-neutrino showers lead to collimated and directional
air-showers offering a new Neutrino Astronomy. At greater energy around PeV,
Tau escaping mountains and Earth and decaying in flight are effectively
showering in air sky. These Horizontal showering is splitting by geomagnetic
field in forked shapes. Such air-showers secondaries release amplified and
beamed gamma bursts (like observed TGF), made also by muon and electron pair
bundles, with their accompanying rich Cherenkov flashes. Also planet' s largest
(Saturn, Jupiter) atmosphere limbs offer an ideal screen for UHE GZK and
Z-burst tau neutrino, because their largest sizes. Titan thick atmosphere and
small radius are optimal for discovering up-going resonant Glashow resonant
showers. Earth detection of Neutrino showering by twin Magic Telescopes on top
mountains, or by balloons and satellites arrays facing the limbs are the
simplest and cheapest way toward UHE Neutrino Astronomy .Comment: 4 pages, 7 figures; an author's name correction and Journal Referenc
Neutrino Astronomy and Cosmic Rays Spectroscopy at Horizons
A new air-showering physics may rise in next years at horizon, offering at
different angles and altitudes a fine tuned filtered Cosmic Rays astrophysics
and an upward Neutrino induced air-showering astronomy. Most of this
opportunity arises because of neutrino masses, their mixing and the consequent
replenishment of rarest tau flavor during its flight in Space. Horizontal air
atmosphere act as a filter for High energy Cosmic Rays (CR) and as a beam dump
for Ultra High Energy (UHE) neutrinos and a powerfull amplifier for its tau
decay in air by its wide showering areas. Earth sharp shadows plays the role of
a huge detector volume for UHE neutrino and a noise-free screen for upcoming
EeVs tau air-showers (as well PeVs anti-neutrino electron air interactions).
Projects for Tau Airshowers are growing at the top of a mountains or at the
edge of a cliff. ASHRA in Hawaii and CRNTN in Utah are tracking fluorescence
lights, while other novel projects on Crown array detectors on mountains, on
balloons and satellites are elaborated for Cherenkov lights. AUGER, facing the
Ande edges, ARGO located within a deep valley are testing inclined showers;
MILAGRO (and MILAGRITO) may be triggered by horizontal up-going muon bundles
from the Earth edges; HIRES and AUGER UHECR detectors, linking twin array
telescopes along their axis may test horizontal Cerenkov blazing photons. MAGIC
(Hess, Veritas) and Shalon Telescopes may act already like a detector for few
PeVs and Glashow resonance neutrino events; MAGIC pointing downward to
terrestrial ground acts as a massive tens of km^3 detector, making it the most
sensitive dedicated neutrino telescope. MAGIC facing the sea edges must reveal
mirrored downward UHECR Air-showers Cherenkov flashes. Magic-crown systems may
lead to tens km^3, neutrino detectors.Comment: 24 pages, 24 figures, Conference NO-VE, Venice, 09-02-200
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