253 research outputs found
An apparent GRBs evolution around us or a sampling of thin GRB beaming jets?
The gamma ray burst apparent average isotropic power versus their red-shift
of all known GRB (Sept.2009) is reported. It calls for an unrealistic Gamma Ray
Burst Evolution around us or it just probe the need of a very thin gamma
precession-jet model. These precessing and spinning jet are originated by
Inverse Compton and-or Synchrotron Radiation at pulsars or micro-quasars
sources, by ultra-relativistic electrons. These Jets are most powerful at
Supernova birth, blazing, once on axis, to us and flashing GRB detector. The
trembling of the thin jet (spinning, precessing, bent by magnetic fields)
explains naturally the observed erratic multi-explosive structure of different
GRBs and its rare re-brightening. The jets are precessing (by binary companion
or inner disk asymmetry) and decaying by power law on time scales to a few
hours. GRB blazing occurs inside the observer cone of view only a seconds
duration times; because relativistic synchrotron (or IC) laws the jet angle is
thinner in gamma but wider in X band. Its apparent brightening is so well
correlated with its hardness (The Amati correlation). This explain the wider
and longer X GRB afterglow duration and the (not so much) rare presence of
X-ray precursors well before the apparent main GRB explosion. The jet lepton
maybe originated by an inner primary hadron core (as well as pions and muons
secondary Jets). The EGRET, AGILE and Fermi few hardest and late GeV gamma
might be PeV neutron beta decay in flight observed in-axis under a relativistic
shrinkage.Comment: 13 pages, 11 figures, Vulcano 200
Inconsistence of super-luminal Cern-Opera neutrino speed with observed SN1987A burst and neutrino mixing for any imaginary neutrino mass
We tried to fit in any way the recent Opera-Cern claims of a neutrino
super-luminal speed with observed Supernova SN1987A neutrino burst and all (or
most) neutrino flavor oscillation. We considered three main frame-works: (1) A
tachyon imaginary neutrino mass, whose timing is nevertheless in conflict with
observed IMB-Kamiokande SN1987A burst by thousands of billion times longer. (2)
An ad hoc anti-tachyon model whose timing shrinkage may accommodate SN1987A
burst but greatly disagree with energy independent Cern-Opera super-luminal
speed. (3) A split neutrino flavor speed (among a common real mass relativistic
neutrino electron component and a super-luminal neutrino {\mu}) in an ad hoc
frozen speed scenario that is leading to the prompt neutrino de-coherence and
the rapid flavor mixing (between electron and muon ones) that are in conflict
with most oscillation records. Therefore we concluded that an error must be
hidden in Opera-Cern time calibration (as indeed recent rumors seem to
confirm). We are also reminding the relevance of the guaranteed minimal
atmospheric neutrino mass whose detection may be achieved by a milliseconds
graviton-neutrino split time delay among gravity burst and neutronization
neutrino peak in any future SN explosion in Andromeda recordable in Megaton
neutrino detector.Comment: 5 pages, 4 figures, corrected and updated atmospheric neutrino
simulatio
The XRF080109-SN2008D and a decade of GRB-Jet-SN connection
Last and nearest GRB-XRF 080109 has been an exceptional lesson on GRB nature.
After a decade (since 25 April 08) we know that Supernovae may often contain a
Jet. Its persistent activity may shine on axis as a GRBs. Such a persistent,
thin beamed gamma jet may be powered by either a BH (Black Holes) or Pulsars.
Late stages of these jets may loose the SN traces and appear as a short GRB or
a long orphan GRB (depending on jet angular velocity and view angle). XRF are
peripherical viewing of the jets. These precessing and spinning gamma jet are
originated by Inverse Compton and-or Synchrotron Radiation at pulsars or
micro-quasars sources, by ultra-relativistic electrons. These Jets are most
powerful at Supernova birth, blazing, once on axis, to us and flashing GRB
detector. The trembling of the thin jet explains naturally the observed erratic
multi-explosive structure of different GRBs. The jets are precessing (by binary
companion or inner disk asymmetry) and decaying by power on time scales of few
hours, but they keep staying inside the observer cone view only a few seconds
duration times (GRB); the jet is thinner in gamma and wider in X band. This
explain the wider and longer X GRB afterglow duration and the rare presence of
X-ray precursors.Comment: 11 pages, 12 figure
Why Tau First?
Electron neutrino has been the first neutral lepton to be foreseen and
discovered last century. The un-ordered muon and its neutrino arose later by
cosmic rays. The tau discover, the heaviest, the most unstable charged lepton,
was found surprisingly on 1975. Its neutrino was hardly revealed just on 2000.
So why High Energy Neutrino Astronomy should rise first via tau neutrino, the
last, the most rare one? The reasons are based on a chain of three favorable
coincidences found last decade: the neutrino masses and their flavor mixing,
the UHECR opacity on Cosmic Black Body (GZK cut off on BBR), the amplified tau
air-shower decaying in flight. Indeed guaranteed UHE GZK tau neutrinos, feed by
muon mixing, while skimming the Earth might lead to boosted UHE tau, mostly
horizontal ones. These UHE lepton decay in flight are spread, amplified, noise
free Air-Shower: a huge event for an unique particle. To be observed soon:
within Auger sky, in present decade. Its discover may sign of the first tau
appearance.Comment: 8 pages, 4 figure
Beaming Selection and SN-GRB-Jets Evolution
After a decade of Fireball reign there is a hope for thin collimated Jet to
solve the Supernova-GRB mysteryComment: 8 pages, 10 figures; white pages 200
UHECR bending, clustering and decaying feeding gamma anisotropy
Ultra High Energy Cosmic Rays (UHECR), made mostly by Helike lightest nuclei might fit the observed spread clustering along Cen-A; He like
UHECR nuclei explain also Virgo absence because these light nuclei fragility and
opacity above a few Mpc. UHECR He from Cen-A AGN being fragile should partially fragment into secondaries at tens EeV multiplet (D, 3He, p) as it appears in a
twin multiplet discovered (AUGER-ICRC-2011), at 20 EeV along the same Cen-A
UHECR clustering. We suggest that UHECR are also (possibly mostly) heavy radioactive galactic nuclei as 56Ni, 57Ni and 57Co, 60Co 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 PeVs electrons and consequent synchrotron TeVs gamma offering UHECR-TeV
correlated wide area sky anisotropy. Additional electron and tau neutrinos secondaries at PeVs might be the first signature of such expected radioactive secondary
tail. Being smeared such decayed neutrinos will be hardly clustered in small scale
Lightest Nuclei in UHECR versus Tau Neutrino Astronomy
UHECR may be either nucleons or nuclei; in the latter case the Lightest
Nuclei, as He, Li, Be, explains at best the absence of Virgo signals and the
crowding of events around Cen-A bent by galactic magnetic fields. This model
fit the observed nuclear mass composition discovered in AUGER. However UHECR
nucleons above GZK produce EeV neutrinos while Heavy Nuclei, as Fe UHECR do not
produce much. UHECR He nuclei at few tens EeV suffer nuclear fragmentation
(producing low energetic neutrino at tens PeVs) but it suffer anyway photo-pion
GZK suppression (leading to EeV neutrinos) once above one-few 10^{20} eV. Both
these cosmogenic UHE secondary neutrinos signals may influence usual predicted
GZK Tau Neutrino Astronomy in significant and detectable way; the role of
resonant antineutrino electron-electron leading to Tau air-shower may also
rise.Comment: 5 pages, 5 figures, CRIS 200
Foreseeing Neutrino spectra in Deep Core
Atmospheric muon neutrino in Deep Core (whose rate and spectra might be soon
available) should exhibit a suppression (due to tens GeV up-going muon neutrino
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. 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.Comment: 8 pages, 8 figure
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