Ultra High Energy, UHE, upward Tau neutrinos nutau , ¯nutau , above hundred TeVs and up to tens P... more Ultra High Energy, UHE, upward Tau neutrinos nutau , ¯nutau , above hundred TeVs and up to tens PeV energies, of relevant astrophysical nature, may lead to UHE Taus and consequent Up-ward Tau air-Showers (UPTAUS) after interaction on Earth crust surface. The UPTAUS discover may open a new UHE Tau Neutrino Astrophysics. A new generation of Gamma, X, optical and Radio Arrays in Space may discover, in the same Auger spirit, such up-coming Airshowers as well as an additional Tau signal: the nearly Horizontal Tau AIR-Shower (HORTAUS) originated by UHE neutrinos tau at 1019 eV energies arising from a thin Earth crust corona at few tens of degree below the horizons; a degree above the horizons, there should be over common diffused cosmic ray albedo, an additional High Altitudes (nearly Horizontal) Showers (HIAS), by more common Cosmic Rays primaries at PeVs up to EeV and ZeV energies, both of hadronic or of electro-magnetic gamma nature. Mini-arrays detectors in high Altitude Balloons tail...
High Energy Neutrino Astronomy has been revealed by a sudden change in the flavor composition aro... more High Energy Neutrino Astronomy has been revealed by a sudden change in the flavor composition around maximal energies since three years of recording in ice km detector. However these discover didn' t led to any clear promised Neutrino Astronomy land yet. No correlation with hard gamma sources was found. Moreover the astrophysical spectra expected at Fermi value, seem to converge to a softer value, also required to avoid any Glashow resonant neutrino signal. We suggest a main solution within a composite flux ruled by prompt atmospheric neutrinos. Nevertheless the recent discover of twentyone crossing muons at hundreds TeVs had shown a first narrow overlapped doublet and a correlated track with a peculiar hard UHECR event clustering pointing to a well known microjet in bynary precession; these first connections hint for a non negligible astrophysical component making neutrino astronomy anyway already more than a hope.
Gamma Ray Burst has been widely believed in last decade to be super-explosions: the Fireball. We ... more Gamma Ray Burst has been widely believed in last decade to be super-explosions: the Fireball. We are argue on the contrary that GRBs (as well as Soft Gamma Repeaters SGR) are precessing Gamma Jets. We remind the list of contradiction that Fireball and its smaller galactic version, the Magnetar, have to face. In particular the existence of weak isolated X-ray precursor signal before the main Gamma Ray Burst and (rare SGR) events disagree with any explosive, one shoot, scenarios either isotropic or wide-beamed. We interpret them as earlier marginal blazing of outlying X conical Jet tails of precessing, spinning gamma Jet.
ABSTRACT Primordial heavy neutrinos of 4th generation might explain different astrophysical puzzl... more ABSTRACT Primordial heavy neutrinos of 4th generation might explain different astrophysical puzzles: indeed, the simplest 4th neutrino scenario may be still consistent with known 4th neutrino physics, cosmic-ray antimatter and gamma fluxes and signals in underground detectors for very narrow neutrino mass windows (46-47 GeV). We have analyzed extended heavy neutrino models related to the clumpiness of neutrino density, neutrino asymmetry and neutrino decay. We found that in these models the underground signals may be better combined with a cosmic ray im-print leading to wider windows for neutrino mass (46-75 GeV) coinciding with the whole range allowed from the uncertainties of electroweak parameters. pROQWLENIQ TQVELOGO NEJTRINO 4-GO POKOLENIQ W POISKAH SKRYTOJ MASSY k.m. bELOCKIJ, d. fARDVON, m.'. hLOPOW, r.w.kONOPLI k.i. –IBAEW pERWIˆNYE TQVELYE NEJTRINO 4-GO POKOLENIQ MOGUT OB˙QSNQTX RAZLIˆNYE ASTROFIZIˆESKIE ZAGADKI: PROSTEJ-[IJ SCENARIJ S 4-M NEJTRINO WSE E]E SOWMESTIM S FIZIKOJ 4-GO NEJTRINO, DANNYMI PO KOSMIˆESKIM LUˆAM I GAMMA-IZLUˆENI@ I SIGNALAMI W PODZEMNYH DETEKTORAH DLQ OˆENX UZKOGO DIAPAZONA ZNAˆENIJ MASSY NEJTRINO (46-47 g"w). mY PROANALIZIROWALI RAS[IRENNYE MODELI TQVELYH NEJTRINO, SWQZANNYE S MELKOMAS[TABNYMI NEODNORODNOSTQMI (KLAMPAMI) RASPREDELENIQ PLOTNOSTI NEJTRINO, ZARQDOWOJ ASIMMETRIEJ I NESTABILXNOSTX@ NEJTRINO. mY NA[LITO W "TIH MODELQH SIGNALY PODZEMNYH "KSPERIMENTOW MOGUTLUE SOˆETATXSQ S SIG-NALAMI W KOSMIˆESKIH LUˆAH, PRIWODQ K BOLEE [IROKOMU DIAPAZONU ZNAˆENIJ MASSY NEJTRINO (46-75 g"w), SOWPADA@]EMU S TAKOWYM, RAZRE[ENNYM SOWOKUPNOSTX@ DANNYH FIZIKI "LEKTROSLABOGO WZAIMODEJSTWIQ.
In the Top-down scenarios, the decay of super-heavy particles (m ∼ 10 GeV ), situated in dark-mat... more In the Top-down scenarios, the decay of super-heavy particles (m ∼ 10 GeV ), situated in dark-matter halos not very far from our Galaxy, can explain the ultra-high-energy (UHE) cosmic-ray spectrum beyond the Griesen-Zatasepin-Kuzmin (GZK) cut-off. In case the dynamics of this decay is governed by the minimal supersymmetric standard model, a major component of the UHE cosmic-ray flux at PeV-EeV energies could be given by the lightest neutralino χ01, that is the lightest stable supersymmetric particle. Then, the signal of UHE χ01’s on earth might emerge over the interactions of a comparable neutrino component. We compute the event rates for the resonant production of right selectrons (ẽR) and right squarks (q̃R) in mSUGRA, when UHE neutralinos of energy Eχ ∼ 10 5 GeV scatter off electrons and quarks in an earth-based detector like IceCube. The production rates and decay widths into the same initial particles χ01e, χ 0 1q turn out to be nearly model independent (the resonance and neutralino physical masses being the only relevant parameters) for the neutralino-electron scattering, and also for the neutralino-nucleon scattering, whenever gluinos are heavier than squarks. We compare the expected number of supersymmetric events with the rates corresponding to the Glashow W resonance and the continuum UHE νN scattering for realistic powerlaw spectra. We find that the supersymmetric event rate can reach a few tens for a one-year exposure in IceCube. Finally, we note that UHE neutralinos at much higher energies (up to hundreds ZeV) may produce sneutrino (ν̃) resonances by scattering off relic neutrinos in the Local Group hot dark halo. The consequent ν̃ burst into hadronic final states could mimic a Z-burst event, but with a quite smaller conversion efficiency.
Ultra High Energy, UHE, upward Tau neutrinos nutau , ¯nutau , above hundred TeVs and up to tens P... more Ultra High Energy, UHE, upward Tau neutrinos nutau , ¯nutau , above hundred TeVs and up to tens PeV energies, of relevant astrophysical nature, may lead to UHE Taus and consequent Up-ward Tau air-Showers (UPTAUS) after interaction on Earth crust surface. The UPTAUS discover may open a new UHE Tau Neutrino Astrophysics. A new generation of Gamma, X, optical and Radio Arrays in Space may discover, in the same Auger spirit, such up-coming Airshowers as well as an additional Tau signal: the nearly Horizontal Tau AIR-Shower (HORTAUS) originated by UHE neutrinos tau at 1019 eV energies arising from a thin Earth crust corona at few tens of degree below the horizons; a degree above the horizons, there should be over common diffused cosmic ray albedo, an additional High Altitudes (nearly Horizontal) Showers (HIAS), by more common Cosmic Rays primaries at PeVs up to EeV and ZeV energies, both of hadronic or of electro-magnetic gamma nature. Mini-arrays detectors in high Altitude Balloons tail...
High Energy Neutrino Astronomy has been revealed by a sudden change in the flavor composition aro... more High Energy Neutrino Astronomy has been revealed by a sudden change in the flavor composition around maximal energies since three years of recording in ice km detector. However these discover didn' t led to any clear promised Neutrino Astronomy land yet. No correlation with hard gamma sources was found. Moreover the astrophysical spectra expected at Fermi value, seem to converge to a softer value, also required to avoid any Glashow resonant neutrino signal. We suggest a main solution within a composite flux ruled by prompt atmospheric neutrinos. Nevertheless the recent discover of twentyone crossing muons at hundreds TeVs had shown a first narrow overlapped doublet and a correlated track with a peculiar hard UHECR event clustering pointing to a well known microjet in bynary precession; these first connections hint for a non negligible astrophysical component making neutrino astronomy anyway already more than a hope.
Gamma Ray Burst has been widely believed in last decade to be super-explosions: the Fireball. We ... more Gamma Ray Burst has been widely believed in last decade to be super-explosions: the Fireball. We are argue on the contrary that GRBs (as well as Soft Gamma Repeaters SGR) are precessing Gamma Jets. We remind the list of contradiction that Fireball and its smaller galactic version, the Magnetar, have to face. In particular the existence of weak isolated X-ray precursor signal before the main Gamma Ray Burst and (rare SGR) events disagree with any explosive, one shoot, scenarios either isotropic or wide-beamed. We interpret them as earlier marginal blazing of outlying X conical Jet tails of precessing, spinning gamma Jet.
ABSTRACT Primordial heavy neutrinos of 4th generation might explain different astrophysical puzzl... more ABSTRACT Primordial heavy neutrinos of 4th generation might explain different astrophysical puzzles: indeed, the simplest 4th neutrino scenario may be still consistent with known 4th neutrino physics, cosmic-ray antimatter and gamma fluxes and signals in underground detectors for very narrow neutrino mass windows (46-47 GeV). We have analyzed extended heavy neutrino models related to the clumpiness of neutrino density, neutrino asymmetry and neutrino decay. We found that in these models the underground signals may be better combined with a cosmic ray im-print leading to wider windows for neutrino mass (46-75 GeV) coinciding with the whole range allowed from the uncertainties of electroweak parameters. pROQWLENIQ TQVELOGO NEJTRINO 4-GO POKOLENIQ W POISKAH SKRYTOJ MASSY k.m. bELOCKIJ, d. fARDVON, m.'. hLOPOW, r.w.kONOPLI k.i. –IBAEW pERWIˆNYE TQVELYE NEJTRINO 4-GO POKOLENIQ MOGUT OB˙QSNQTX RAZLIˆNYE ASTROFIZIˆESKIE ZAGADKI: PROSTEJ-[IJ SCENARIJ S 4-M NEJTRINO WSE E]E SOWMESTIM S FIZIKOJ 4-GO NEJTRINO, DANNYMI PO KOSMIˆESKIM LUˆAM I GAMMA-IZLUˆENI@ I SIGNALAMI W PODZEMNYH DETEKTORAH DLQ OˆENX UZKOGO DIAPAZONA ZNAˆENIJ MASSY NEJTRINO (46-47 g"w). mY PROANALIZIROWALI RAS[IRENNYE MODELI TQVELYH NEJTRINO, SWQZANNYE S MELKOMAS[TABNYMI NEODNORODNOSTQMI (KLAMPAMI) RASPREDELENIQ PLOTNOSTI NEJTRINO, ZARQDOWOJ ASIMMETRIEJ I NESTABILXNOSTX@ NEJTRINO. mY NA[LITO W "TIH MODELQH SIGNALY PODZEMNYH "KSPERIMENTOW MOGUTLUE SOˆETATXSQ S SIG-NALAMI W KOSMIˆESKIH LUˆAH, PRIWODQ K BOLEE [IROKOMU DIAPAZONU ZNAˆENIJ MASSY NEJTRINO (46-75 g"w), SOWPADA@]EMU S TAKOWYM, RAZRE[ENNYM SOWOKUPNOSTX@ DANNYH FIZIKI "LEKTROSLABOGO WZAIMODEJSTWIQ.
In the Top-down scenarios, the decay of super-heavy particles (m ∼ 10 GeV ), situated in dark-mat... more In the Top-down scenarios, the decay of super-heavy particles (m ∼ 10 GeV ), situated in dark-matter halos not very far from our Galaxy, can explain the ultra-high-energy (UHE) cosmic-ray spectrum beyond the Griesen-Zatasepin-Kuzmin (GZK) cut-off. In case the dynamics of this decay is governed by the minimal supersymmetric standard model, a major component of the UHE cosmic-ray flux at PeV-EeV energies could be given by the lightest neutralino χ01, that is the lightest stable supersymmetric particle. Then, the signal of UHE χ01’s on earth might emerge over the interactions of a comparable neutrino component. We compute the event rates for the resonant production of right selectrons (ẽR) and right squarks (q̃R) in mSUGRA, when UHE neutralinos of energy Eχ ∼ 10 5 GeV scatter off electrons and quarks in an earth-based detector like IceCube. The production rates and decay widths into the same initial particles χ01e, χ 0 1q turn out to be nearly model independent (the resonance and neutralino physical masses being the only relevant parameters) for the neutralino-electron scattering, and also for the neutralino-nucleon scattering, whenever gluinos are heavier than squarks. We compare the expected number of supersymmetric events with the rates corresponding to the Glashow W resonance and the continuum UHE νN scattering for realistic powerlaw spectra. We find that the supersymmetric event rate can reach a few tens for a one-year exposure in IceCube. Finally, we note that UHE neutralinos at much higher energies (up to hundreds ZeV) may produce sneutrino (ν̃) resonances by scattering off relic neutrinos in the Local Group hot dark halo. The consequent ν̃ burst into hadronic final states could mimic a Z-burst event, but with a quite smaller conversion efficiency.
High Energy Neutrino Astronomy has been revealed by a sudden change in the flavor composition abo... more High Energy Neutrino Astronomy has been revealed by a sudden change in the flavor composition above 30 TeV since 2013 by IceCube detector: the fast growth of spherical showers over atmospheric muon track signal in IceCube marked the revolution. However these discover didn't led to the promised Neutrino-Astronomy-Land yet. AGN flaring are not correlated with these high energy tens TeV-PeV events. Brightest persistent or pulsed galactic sources are missing while no point source arise in the lower energy sky. GRB events do not correlate within any minute-hour lapse time windows along any neutrino event. Moreover the astrophysical hard spectra whose exponent was expected at Fermi value of −2, seem to converge from −2.2 to a softer −2.7 or −3.0 value, also needed to avoid unobserved Glashow resonant neutrino at 6.3 PeV energy. Finally a key question arises: why within the ten UHE neutrino, those harder than 200 TeV events (whose timing structure would allow IceCube to disentangle any double tau neutrino imprint) don't double bang anyway? We suggest a main solution within a composite flux mostly ruled by prompt atmospheric neutrinos. Nevertheless in the very recent discover of 21 through-going (crossing) muons at hundreds TeVs, whose tracks are more aligned and telling, is shown a first narrow doublet (and some of correlated UHECR clustered source); this points – or give hints – for a non-negligible 10 − 20% astrophysical component, making neutrino astronomy already alive anyway.
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Papers by Daniele Fargion