arXiv subjects

D. Fargion

Publications and source records attributed to D. Fargion.

At least 55 records · Page 3Linked to original sources

arXiv2006

Air-Showers in Space and Z-Showers in Universe for Neutrino Astronomy and Spectroscopy

Amplified Tau-airshower at horizons may well open a novel powerful windows, at PeV-EeV energy, to Neutrino Astronomy. Neutrino induced air-showering astronomy rise because of neutrino masses, their mixing and the consequent replenishment of tau flavor during neutrino flight into spaces; Tau-Air-Showers escaping the Earth are the main traces amplified by its millions muon, billions gamma and thousand billions photon secondaries. Earth edges and its sharp shadows is the huge beam-dump detector for UHE neutrino and the almost noise-free screen for tau air-showers (as well as for PeVs anti-neutrino electron scattering on air electrons by resonant interactions). Crown array detectors for horizontal Cherenkov signals on mountains, on balloons and satellites widening the solid angle view are being elaborated; deep and wide valleys are considered. MAGIC Telescopes pointing downward to terrestrial grounds acts, for EeV Tau neutrino air-showers astronomy, as a massive tens of km^3 water equivalent detector, making (in a given direction) it at present the most powerful dedicated neutrino telescope at PeVs. MAGIC facing the sea edges must also reveal mirrored downward UHECR Air-showers (Cherenkov) flashes. Magic-crown systems may lead to largest neutrino detectors in near future. They maybe located on top mountains, on planes or balloons or in satellite arrays. They may be screened in deep valleys. MILAGRO (and past MILAGRITO or future larger detectors) on a mountain top might already hide records of horizontal up-going muon bundles due to far UHECR and less far (but rarer) tau air-showers at EeV. UHE neutrino may also scatter on relic light (0.1-0.2 eV) ones, showering in the Universe at ZeV energies Cosmic Rays.

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arXiv2006

GRBs, SGRs by UHE leptons showering, blazing and re-brightening by precessing Gamma Jets in-off axis

A list of questions regarding Gamma Ray Bursts (GRBs) and Soft Gamma Repeaters (SGRs) remain unanswered within the Fireball-cone and Magnetar explosive scenarios. A persistent, thin (less than micron-sr solid angle) precessing and spinning gamma jet, with a power output comparable to the progenitor supernova (SN) or XRay pulsar, may explain these issues. The precessing jets may have a few hours characteristic decay time, while their decreasing intensity follow a power law for thousands of years. The orientation of the spinning and precessing beam respect to the line of sight plays a key role : the farthest GRB events in widest cosmic volumes correspond generally to a very narrow and on-axis beam, while for the nearest ones sources are mostly observable off-axis. Consequentely the far ones are the hardest and the most bright and viceversa nearest one are mostly softer and longest ones as in Amati correlation. We expect that nearby off-axis GRBs would be accompanied by a chain of OT and radio bumps as in GRB030329-SN2003 and latest GRB060218-SN2006 events. Delayed blazing jets are observable in the local universe as X-Ray Flahes (XRFs) or short GRBs often as orphan afterglow event, and at closer distances as SGRs and anomalous X-ray Pulsars AXRPs. The gamma jet is originated by ultra-relativistic electron pairs showering via Synchrotron (or Inverse Compton) radiation. The electron pairs escape from the inner SN core thanks to a more penetrating couriers, the relativistic PeV muon pairs, themselves secondaries of inner UHE hadron jets. They are 'transparent' through the SN shells of matter and lights; they decay far away in to electron pairs (and later on) in gamma and neutrinos jets. Then GRBs (and SGRs) are not the most explosive event of the Universe, but just the most beamed ones.

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arXiv2006

Anti-Neutrino Imprint in Solar Neutrino Flare

Future neutrino detector at Megaton mass might enlarge the neutrino telescope thresholds revealing cosmic supernova background and largest solar flares neutrino. Indeed the solar energetic flare particles while scattering among themselves on Solar corona atmosphere must produce prompt charged pions, whose chain decays are source of solar (electron-muon) neutrino "flare" (at tens or hundreds MeV energy). These brief (minutes) neutrino "burst" at largest flare peak may overcome by three to five order of magnitude the steady atmospheric neutrino noise on the Earth, possibly leading to their detection above detection. Moreover the birth of anti-neutrinos at a few tens MeVs is well loudly flaring above a null thermal "hep" anti-neutrino solar background and also above a tiny supernova relic and atmospheric noise. The largest prompt solar anti-neutrino "burst" may be well detected in future SuperKamikande (Gadolinium implemented) by anti-neutrino signatures mostly in inverse Beta decay. Our estimate for the recent and exceptional October - November 2003 solar flares and January 20th 2005 exceptional eruption might lead to a few events above or near unity for existing Super-Kamiokande and above unity for Megaton detectors. The neutrino spectra may reflect in a subtle way the neutrino flavor oscillations and mixing in flight. A comparison of the solar neutrino flare (at their birth place on Sun and after oscillation on the arrival on the Earth) with other neutrino foreground is estimated: it offers an independent track to disentangle the neutrino flavor puzzles and its most secret mixing angles. The sharpest noise-free anti-neutrino imprint maybe its first clean voice.

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arXiv2006

Crown Detectors to Observe Horizontal and Upward Air-Showers

Cerenkov Telescopes and Scintillators set on a Crown-like arrays facing the Horizons may reveal far Cosmic Rays Showers, nearer Anti-Neutrino-Electron + Electron --> W- shower in air and upgoing Tau Neutrino + N--> tau + X, --> Shower, Earth-Skimming tau air-showers. Even UHE SUSY Chi + e--> Selectron--> Chi + e at tens PeVs-EeV energy may blaze at Horizons, as anti-neutrino electron at Glashow peak - Burst shower. We show first estimate on down and up-going Horizontal Showers traces for present and future Magic-like Crown Arrays and their correlated Scintillator-like twin Crown Arrays. The one mono or stereo-Magic elements facing the Horizons are already comparable to present Amanda underground neutrino detector.

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arXiv2006

Study of a detector array for Upward Tau Air-Showers

The cosmic ray spectrum extends to energies above 10^20 eV. In direct production or acceleration models, as well as by photo-pion interaction high energy cosmic ray flux must contain neutrinos and photons. The latter are absorbed by cosmic radiations while neutrinos are not. The need of a Neutrino Astronomy is compelling. In this paper a study of a detector array designed to measure horizontal tau air-showers emerging from the ground, produced by nu_tau interactions with the Earth's crust, is presented. Each array unit is composed of a pair of scintillator tiles mounted on a frame with a front field of view of about 0.1 sr, optimized to distinguish between up-going and down-going crossing particles by their time of flight. The detector array sensitivity, the size of the array and the tau shower identification are discussed. Because of the almost complete mixing of nu_mu to nu_tau the ultrahigh energy neutrino tau and its minimal consequent tau-airshower rate is estimated; assuming that the neutrino energy spectrum follows a Fermi-like power law E^-2, the sensitivity with 3 years of observation is estimated to be about 60 eV cm^-2s^-1sr^-1 in the energy range 10^{17-20} eV. This value would provide competitive upper limit with present and future experiments. We found also that, in the same time, this system can observe about one GZK neutrino event per km^2.

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arXiv2005

Is FLARE for Solar flare?

The Fermi Lab Liquid ARgon experiment, FLARE, a huge neutrino argon-liquid project detector of 50 kt mass, might in a near future enlarge the neutrino telescope accuracy revealing in detail solar, supernova, atmospheric as well as largest solar flares neutrino. Indeed the solar energetic (E_p > 100 MeVs) flare particles (protons, alpha) while scattering among themselves or hitting the solar atmosphere must produce on sun prompt charged pions, whose decay (as well as their sequent muon decays) into secondaries is source of a copious solar neutrino "flare" (at tens or hundreds MeV energy). These brief (minutes) neutrino "burst" at largest flare peak may overcome by three to five order of magnitude the steady atmospheric neutrino noise on the Earth, possibly leading to their emergence and detection above the thresholds. The largest prompt "burst" solar neutrino flare may be detected in future FLARE neutrino detectors both in electron and positron and possibly in its muon pair neutrino component. Our estimate for the recent and exceptional October - November 2003 solar flares and last January 20th 2005 exceptional flare might lead to a few events for future FLARE or near unity for present Super-KamiokandeII. The neutrino spectra may reflect the neutrino flavor oscillations and mixing in flight. In neutrino detectors a surprising (correlated) muon appearance may occur while a rarer tau appearance may even marginally take place. A comparison of the solar neutrino flare signal with other neutrino foreground is estimated: it offer the first opportunity for an independent road map to disentangle the neutrino flavor puzzles, as well a prompt alarm system for dangerous solar flare eruptions.

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arXiv2005

May Gravity detect Tsunami ?

The present gravitational wave detectors are reaching lowest metric deviation fields able to detect galactic and extra-galactic gravitational waves, related to Supernova explosions up to Virgo cluster. The same gravitational wave detector are nevertheless almost able to reveal, in principle, near field Newtonian gravitational perturbations due to fast huge mass displacements as the ones occurring during largest Earth-Quake or Tsunami as the last on 26nd December 2004 in Asiatic area. Virgo and Ligo detector are unfortunately recording on high frequencies (above tens Hz) while the signal of the Tsunami lay at much lower range (below 0.1 Hz). Nevertheless prompt gravitational near field deformation by the Tsunami might reach the future LISA threshold sensitivity and frequency windows if such an array is located nearby (3000-10000) km distances. Unfortunately the present LISA system should be located at Lagrange point too far (1.5 million km. far away). We note however that the later continental mass rearrangement and their gravitational field assessment on Earth must induce, for Richter Magnitude 9-like Tsunami, a different terrestrial inertia momentum and a different principal rotation axis. In conclusion we remind that gravitational geodetic deviation on new precise satellites (GOCE 2006), assisted by GPS network, might nevertheless reach in the near future the needed threshold and accuracy to reveal Tsunami by their prompt tidal gravity field deviations . An array of such geoid detector maybe correlated with LISA-like satellite on Earth orbits may offer the fastest alarm system.

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arXiv2005

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.

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arXiv2005

Tera-Leptons Shadows over Sinister Universe

The role of Sinister Heavy Fermions in recent Glashow's SU(3)*SU(2)*SU(2)'*U(1) model is to offer in a unique frame relic Helium-like products (an ingenious candidate to the dark matter puzzle), a solution to the See-Saw mechanism for light neutrino masses as well as to strong CP violation problem in QCD. The Sinister model requires a three additional families of leptons and quarks, but only the lightest of them Heavy U-quark and E-"electron" are stable. Final neutral Helium-like UUUEE state is an ideal evanescent dark-matter candidate. However it is reached by multi-body interactions along a tail of more manifest secondary frozen blocks. They should be now here polluting the surrounding matter. Moreover, in opposition to effective pair quark annihilations, there is no such an early or late tera-lepton pairs suppressions, because:a) electromagnetic interactions are "weaker" than nuclear ones and b) helium ion 4He++ is able to attract and capture, E-, fixing it into a hybrid tera helium "ion" trap. This leads to a pile up of relic (4HeE)+ traces, a lethal compound for any Sinister Universe. This capture leaves no Tera-Lepton frozen in Ep relic (otherwise an ideal catalyzer to achieve effective late E+E- annihilations possibly saving the model). The (4HeE)+ Coulomb screening is also avoiding the synthesis of the desired UUUEE hidden dark matter gas. The e(4HeE)+ behave chemically like an anomalous hydrogen isotope.Also tera-positronium (eE+) relics are over-abundant and they behave like an anomalous hydrogen atom: these gases do not fit by many orders of magnitude known severe bounds on hydrogen anomalous isotope, making grave shadows over a Sinister Universe. However a surprising and resolver role for Tera-Pions in UHECR astrophysics has been revealed.

hep-ph↗

arXiv2005

Neutrino Astronomy beyond and beneath the Horizons

The Earth's Shadow to Cosmic Rays offer a windows to Tau Neutrino Astronomy at the Horizon edges. Inclined and Horizontal C.R. Showers (70^o-90^o zenith angle) produce secondary (gamma,e) mostly suppressed by high column atmosphere depth. The shower Cherenkov photons are diluted and filtered by air opacity, but secondary penetrating, muon pairs and their decay into electron pairs, revive additional Cerenkov flash lights. Most largest GeVs gamma telescopes may detect such UHECR horizontal showers. Arrival angle and column depth, shower shape, timing may inform on the altitude interaction and on primary UHECR composition. At larger zenith angle (90^o-99^o) more rare up-going showers are traced by muon (as well electromagnetic) bundles that would give evidence of rare Earth-Skimming neutrinos, tau and anti-tau neutrinos, at PeVs-EeVs energies. Their rate may be comparable with 6.3 PeVs anti-neutrino electron induced air-shower originated in interposed atmosphere, by W^- resonance at Glashow peak. Additional and complementary UHE SUSY neutralino or staus may blaze. Their nature might be disentangled by Stereoscopic Telescopes array. Magic and Hess telescope in present set up may be already comparable to AMANDA underground neutrino detector. Such telescopes pointing at the horizons toward active sources (AGN,BL Lac Objects, GRBs or SGRs blazing micro-quasar jet, and SNRs) do experience in those directions an air mass corresponding to a km^3 water one. Therefore Horizontal Showering is already the most sensitive windows to Neutrino Astronomy possibly pointing to AGN,GRB or SGR events.

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arXiv2005

UHE Leptons and Neutrons feeding Precessing gamma Jet in GRBs - SGRs: A SGR 1806-20 link to EeV C.R.?

Soft Gamma Repeaters are widely believed to occur as isotropic Magnetar explosion. We suggest on the contrary that they may be described by thin collimated spinning and precessing Gamma Jets flashing and blazing along the line of sight. The Jet (for SGRs) maybe powered by an accretion disk in binary system and it reproduces huge outflow and oscillating blazing mode as the observed ones in Giant Flare SGR 1806-20. The precessing and spinning blazing nature reflects at smaller intensity the same behavior observed in brief GRBs Jetted Supernova, as well as re-brightening and bumps in afterglows. The SGR gamma beam maybe powered by Inverse Compton Scattering or by Synchrotron Radiation of electron pair beam respectively at GeVs or PeVs energies. In the latter case tens PeVs leptons (muons and later decaying PeVs electrons) might be originated while EeV nucleons Jets (protons-neutrons) are in photo-pion equilibrium with infrared photons surrounding the source. The neutron Jet might survive and remain collimated. It maybe already detected as an EeV cosmic ray anisotropy in present AGASA map pointing toward known (North Hemisphere) SGRs : SGR 1900 +14 and SGR 1806-20. If the SGR-EeV connection is correct a parasite traces of PeVs neutrino as well PeV-TeVs gamma rays might be found in present or future data records, among the others C.R. array detectors, inside the Amanda and Milagro volumes.

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arXiv2005

GRBs and SGRs by high energy leptons showering in blazing gamma jets: are SGRs sources of EeV CRs?

The apparently huge energy budget of the gamma ray burst GRB 990123 led to the final collapse of the isotropic fireball model, forcing even the most skeptical to consider a beamed Jet emission correlated to a supernova (SN) explosion. Similarly the surprising giant flare from the soft gamma repeater SGR 1806-20 that occurred on 2004 December 27, may induce the crisis of the magnetar model. If the apparently huge energy associated to this flare has been radiated isotropically, the magnetar should have consumed at once most of (if not all) the energy stored in the magnetic field. On the contrary we think that a thin collimated precessing jet, blazing on-axis, may be the source of such apparently huge bursts with a moderate output power. We discuss the possible role of the synchrotron emission and electromagnetic showering of PeV electron pairs from muon bundles. A jet made of muons may play a key role in avoiding the opacity of the SN-GRB radiation field. We propose a similar mechanism to explain the emission of SGRs. In this case we also examine the possibility of a primary hadronic jet that would produce ultra relativistic e+ e- (1 - 10 PeV) from pion- muon or neutron decay. Such electron pairs would emit a few hundreds keV radiation from their interaction with the galactic magnetic field, as it is observed in the intense gamma ray flare from SGR 1806-20. A thin precessing jet from a pulsar may naturally explain the negligible variation of the spin frequency. A correlation between SGR 1806-20, SGR 1900 +14, Cygnus and the AGASA excess of EeV cosmic rays (CRs) has been found; we suggest that a robust EeV signal may be detected by AUGER or Milagro in the near future.

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arXiv2005

Cosmic Rays Astrophysics and Neutrino Astronomy beyond and beneath the Horizons

Modern Terrestrial Cerenkov Telescopes and Array Scintillators facing the Horizons may soon reveal far Cosmic Rays or nearer PeVs-EeVs Neutrino Showers Astronomy. Indeed UHE neutrino interactions in air, leading to Horizontal Showers, may take place through several channels: the main Glashow resonant one, the charged nuclear interactions and the neutral current events. Analogous events occur also for the neutrino-nucleon events. These interactions are producing hadronic or electromagnetic showers at the far horizons and their correlated secondaries Cerenkov flashes. Comparable interactions are producing, inside the Earth, the Horizontal, but Up-going ultra-relativistic tau, whose decay in flight is source of tau Air Showers (Uptaus and HorTaus); Horizontal Tau Air-Showers are rarely (one-two order of magnitude) enhanced by highest mountain chains at horizons, as in AUGER experimental site; their hadronic or electromagnetic traces are preferentially at PeV-EeV energies; their tracks are amplified by their muon-gamma bundles whose signals are above the random noises and better disentangled by Cerenkov flashes in time coincidence. More exotic UHE SUSY interactions at tens PeVs-EeV energy may blaze at Horizons. Anyway common High Energy Cosmic rays at PeVs-EeVs energy must traces their presence in Magic-like Cerenkov Telescopes at horizons. Present Magic Telescopes facing the Horizons are, at equal given time, almost comparable with the Amanda underground neutrino detector.

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arXiv2005

GRBs-SN and SGR-X-Pulsar as blazing Jets

Old and recent puzzles of GRBs and SGRs find a solution with a model based on the fast blazing of very collimated thin gamma Jets. Damped oscillating afterglows in GRB030329 find a natural explanation assuming a very thin Jet whose persistent activity and different angle of view maybe combined at once with the Supernovae power and the apparent huge GRBs output. The same thin beaming offer an understanding of the apparent SGR-Pulsar power connection. A thin collimated precessing Gamma Jet model for both GRBs and SGRs, at their different scaled luminosity (10^{44} - 10^{38}erg s^-1), explains the existence of few identical energy spectra and time evolution of these sources leading to a unified model. Their similarity with the huge precessing Jets in AGN, QSRs and Radio-Galaxies inspires this smaller scale SGR-GRB model. The spinning-precessing Jet explains the rare mysterious X-Ray precursors in GRBs and SGRs events. Any large Gamma Jet off-axis beaming to the observer might lead to the X-Flash events without any GRB signals, as the most recent XRF030723. Its possible re-brightening would confirm the evidence of the variable pointing of the jet in or off line towards the observer. Indeed a multi-precessing Jet at peak activity in all bands may explain the puzzling X or optical re-brightening bumps found in the GRB 021004, GRB030329 and the SGR 1900+ 14 on 27 August 1998 and once again on the 18 April 2001. Rarest micro-quasars neutron star in our galaxy as SS433, and Herbig Haro objects and Cir-X-1 describe these thin precessing Jet imprints in the spectacular shapes of their relic nebulae.

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arXiv2005

Rates of Horizontal Tau Air-Showers observable by satellites

Up-going and Horizontal Tau Air-Showers, UpTaus and HorTaus, may trace Ultra High Energy Neutrino Tau Earth Skimming at the edge of the horizon. We show that such events even for minimal GZK neutrino fluxes could be detected by space telescopes such as the EUSO project. These Horizontal Tau Showers will track very long fan-like, multi-finger showers whose signature would be revealed by EUSO, OWL experiments. Moreover the additional imprint of their young secondaries muon, electron pairs and gamma bundles flashes might allow to disentangle their nature from the older UHECR secondaries in horizontal showers. Indeed at large zenith angles, the muon, electron pairs and gamma number for far and old Ultra High Energy Cosmic Rays, becomes comparable. On the contrary up-ward muon bundles from UpTaus and HorTaus (as well as by anti-neutrino electron + electron resonance at Glashow peak) may arise within a young shower with a gamma-muon ratio as large as 10^2. Such a very characteristic imprint maybe observed by Crown detector arrays on Mountain, planes or balloons in space, as well as by gamma satellites in Space. We estimate the UpTaus and HorTaus rate from the Earth and the consequent event rate of +/-mu bundles, whose flux at 92^o -97^o may exceed the up-going muon flux induced by the atmospheric neutrino, by one or two order of magnitude.

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arXiv2004

Blazing Cerenkov Flashes at the Horizons by Cosmic Rays and Neutrinos Induced Air-Showers

High Energy Cosmic Rays (C.R.) versus Neutrino and Neutralino induced Air-Shower maybe tested at Horizons by their muons, gamma and Cerenkov blazing signals. Inclined and Horizontal C.R. Showers (70-90 zenith angle) produce secondary (gamma, e+, e-) mostly suppressed by high column atmosphere depth. Earliest shower Cherenkov photons are diluted by large distances and by air opacity, while secondary penetrating muons and their successive decay into electrons and gamma, may revive additional Cerenkov lights. GeVs gamma telescopes at the top of the mountains or in Space may detect at horizons PeVs up to EeV C.R. and their secondaries. Details on arrival angle and column depth, shower shape, timing signature of photon flash intensity, may inform us on the altitude interaction and primary UHECR composition. Below the horizons, at zenith angle among copious single albedo muons, rare up-going showers traced by muon bundles would give evidence of rare tau Earth-Skimming neutrinos, at EeVs energies. Their rate may be comparable with 6.3 PeVs anti-neutrino electron induced air-shower (mostly hadronic) originated above and also below horizons, in interposed atmosphere by W resonance at Glashow peak. Additional and complementary UHE SUSY neutralinos at tens PeVs-EeV energy may blaze, by its characteristic electromagnetic signature. Their secondary shower blazing Cerenkov lights and distances might be disentangled from UHECR by Stereoscopic Telescopes such as Magic ones or Hess array experiment. The horizontal detection sensitivity of Magic in the present set up (if totally devoted to the Horizons Shower search) maybe already be comparable to AMANDA underground neutrino detector at PeVs energies.

astro-ph↗

arXiv2004

May Heavy hadrons of the 4th generation be hidden in our Universe while close to detection?

Metastable quarks of 4th generation are predicted in the framework of heterotic string phenomenology. Their presence in heavy stable hadrons are usually strongly constrained; however their hidden compositions in Heavy doubly charged baryons here considered are found to be still allowable: we studied their primordial quark production in the early Universe, their freezing into cosmic Heavy hadrons, their later annihilation into cosmic ray as well as their relic presence in our Universe and among us on Earth. We discuss also their possible production in present or future accelerators. Indeed if the lightest quarks and antiquarks of the 4th generation are stored in doubly charged baryons and neutral mesons, their lifetime can exceed the age of the Universe; the existence of such an anomalous Helium-like (and neutral Pion-like) stable particles may escape present experimental limits, while being close to present and future experimental test. On the contrary primordial abundance of lightest hadrons of the 4th generation with charge +1 can not decrease below the experimental upper limits on anomalous hydrogen and therefore (if stable) it is excluded. While 4th quark hadrons are rare, their presence may play different and surprising role in cosmic rays, muon and neutrino fluxes and cosmic electromagnetic spectra. Most of these traces are tiny, but just nearly detectable.

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arXiv2004

May Heavy neutrinos solve underground and cosmic ray puzzles?

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 anti-matter and gamma fluxes and signals in underground detectors for a very narrow neutrino mass windows (46-47 GeV). We have analyzed extended Heavy neutrino models related to the clumpiness of neutrino density, new interactions in Heavy neutrino annihilation, neutrino asymmetry, neutrino decay. We found that in these models the underground signals maybe better combined with the cosmic ray imprint leading to a wider windows for neutrino mass (46-75 GeV) coinciding with the whole range allowed from uncertainties of electro-weak parameters.

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