scholarly journals Predictions for the cosmogenic neutrino flux in light of new data from the Pierre Auger Observatory

2007 ◽  
Vol 76 (12) ◽  
Author(s):  
Luis A. Anchordoqui ◽  
Haim Goldberg ◽  
Dan Hooper ◽  
Subir Sarkar ◽  
Andrew Taylor
Keyword(s):  
Neutrino Flux ◽  
Pierre Auger Observatory

scholarly journals The Askaryan Radio Array

2012 ◽  
Vol 8 (S288) ◽  
pp. 115-122
Author(s):  
Kara D. Hoffman
Keyword(s):  
Neutrino Flux ◽  
Austral Summer ◽  
Cosmic Ray ◽  
High Energy ◽  
Pierre Auger Observatory ◽  
Ultra High Energy ◽  
Performance Requirements ◽  
Transparent Media ◽  
Order Of Magnitude ◽  
Cosmic Ray Flux

AbstractUltra high energy cosmogenic neutrinos could be most efficiently detected in dense, radio frequency (RF) transparent media via the Askaryan effect. Building on the expertise gained by RICE, ANITA and IceCube's radio extension in the use of the Askaryan effect in cold Antarctic ice, we are currently developing an antenna array known as ARA (The Askaryan Radio Array) to be installed in boreholes extending 200 m below the surface of the ice near the geographic South Pole. The unprecedented scale of ARA, which will cover a fiducial area of ≈ 100 square kilometers, was chosen to ensure the detection of the flux of neutrinos suggested by the observation of a drop in high energy cosmic ray flux consistent with the GZK cutoff by HiRes and the Pierre Auger Observatory. Funding to develop the instrumentation and install the first prototypes has been granted, and the first components of ARA were installed during the austral summer of 2010–2011. Within 3 years of commencing operation, the full ARA will exceed the sensitivity of any other instrument in the 0.1-10 EeV energy range by an order of magnitude. The primary goal of the ARA array is to establish the absolute cosmogenic neutrino flux through a modest number of events. This information would frame the performance requirements needed to expand the array in the future to measure a larger number of neutrinos with greater angular precision in order to study their spectrum and origins.

scholarly journals Bound on a flux of ultra-high energy neutrinos in a scenario with extra dimensions

2018 ◽  
Vol 191 ◽  
pp. 08010
Author(s):  
Mikhail Astashenkov ◽  
Alexander Kisselev
Keyword(s):  
Energy Range ◽  
Upper Bound ◽  
Extra Dimensions ◽  
Neutrino Flux ◽  
High Energy ◽  
Pierre Auger Observatory ◽  
Ultra High Energy ◽  
Expected Number ◽  
Surface Detector ◽  
Ultra High Energy Neutrinos

Assuming that a single-flavor diffuse neutrino flux dNv/dEv is equal to kE-2v in the energy range 1017 eV - 2:5 × 1019 eV, an upper bound on k is calculated in the ADD model as a function of the number of extra dimensions n and gravity scale MD. An expected number of neutrino induced events at the Surface Detector array of the Pierre Auger Observatory is estimated.

scholarly journals An experimental result coming from Neutrino research gives for all particles the ratio (si /mi) defined by Quantum Inertial theory in conjunction with the Micro-quanta paradigm

2017 ◽  
Vol 9 (6) ◽  
pp. 1
Author(s):  
Maurizio Michelini
Keyword(s):  
National Laboratory ◽  
Neutrino Flux ◽  
Physical Nature ◽  
Empty Space ◽  
Physical Reality ◽  
Experimental Result ◽  
Absolute Space ◽  
Physical Interaction ◽  
Inertial Forces ◽  
Unknown Quantity

Rejecting some old misconceptions (such as the “pulling” gravitation that ravaged classical physics) the Inertial-Gravitational theory supported by the Micro-quanta paradigm incorporates both the relativistic concepts of Mass - Momentum - Energy and the quantic Inertial Model of the particle mass. The flux of micro-quanta supports primarily the physical interaction that generates the Inertial forces defined by Newton. Scholars believing that Inertial forces originate from the properties of the empty space, do not pertain to the community of physicists believing on Newton’s Inertial Law. This great ancient physicist admitted he was unable to explicit the physical nature of his Law of Inertia (“Hypotheses non fingo”). However, marking the difference between “empty” and “absolute” space, he remained in his conviction that some unknown physical reality originates (in the absolute space) the inertial forces upon accelerated masses. At present, Micro-quanta paradigm describes the quantic objects that generate through collisions the physical inertial forces on particles. Since the flux of micro-quanta fills all space, there is no need to refer these collisions to some external System of reference. The relative velocity between quanta and particles comes out from the momentum that micro-quanta confer to particles. By this reason the Micro-quanta paradigm defines on pure dynamical bases the relativistic formalism that Special relativity derived from kinematics, so creating flaws that produced the well known paradoxes. To reveal the micro-quanta it's not necessary to devise particular experiments. The technique of the accelerometers has given many evidences of the physical reality guessed by Newton to explain inertial forces exerted on masses. Since the action of micro-quanta is always manifested in statistical terms, classical and relativistic physics allowed to describe Inertia and Gravitation without knowing the quantic nature of these phenomena. The micro-quanta Paradigm shows in particular the proportionality between cross section and mass (ratio Au) of all particles colliding with micro-quanta. To the aim of calculating the transmission across matter of micro-quanta and neutrinos (which show the same nature) the only unknown quantity is the numerical value of the ratio Au. Recalling that micro-quanta flux fills all space, it appears also interesting to search about neutrino collisions with micro-quanta flux as possible cause of the oscillations phenomena that occur during neutrino travels across the (so called) astronomic “empty” space. A quantitative indication on the ratio Ao is found in this paper from an experimental measurement of the solar neutrino flux interacting with the Earth mass in the course of the Borexino research carried out at Gran Sasso National Laboratory.

scholarly journals LEvEL: Low-Energy Neutrino Experiment at the LHC

2021 ◽  
Vol 2021 (8) ◽  
Author(s):  
Kevin J. Kelly ◽  
Pedro A. N. Machado ◽  
Alberto Marchionni ◽  
Yuber F. Perez-Gonzalez
Keyword(s):  
Cross Sections ◽  
Hadron Collider ◽  
Neutrino Flux ◽  
Coherent Scattering ◽  
Forward Direction ◽  
Low Energy ◽  
Neutrino Experiment ◽  
Beam Dump ◽  
Neutrino Production ◽  
Energy Neutrino

Abstract We propose the operation of LEvEL, the Low-Energy Neutrino Experiment at the LHC, a neutrino detector near the Large Hadron Collider Beam Dump. Such a detector is capable of exploring an intense, low-energy neutrino flux and can measure neutrino cross sections that have previously never been observed. These cross sections can inform other future neutrino experiments, such as those aiming to observe neutrinos from supernovae, allowing such measurements to accomplish their fundamental physics goals. We perform detailed simulations to determine neutrino production at the LHC beam dump, as well as neutron and muon backgrounds. Measurements at a few to ten percent precision of neutrino-argon charged current and neutrino-nucleus coherent scattering cross sections are attainable with 100 ton-year and 1 ton-year exposures at LEvEL, respectively, concurrent with the operation of the High Luminosity LHC. We also estimate signal and backgrounds for an experiment exploiting the forward direction of the LHC beam dump, which could measure neutrinos above 100 GeV.

scholarly journals Starburst galaxies strike back: a multi-messenger analysis with Fermi-LAT and IceCube data

2021 ◽  
Vol 503 (3) ◽  
pp. 4032-4049
Author(s):  
Antonio Ambrosone ◽  
Marco Chianese ◽  
Damiano F G Fiorillo ◽  
Antonio Marinelli ◽  
Gennaro Miele ◽  
...  
Keyword(s):  
Cosmic Rays ◽  
Gamma Ray ◽  
Neutrino Flux ◽  
Data Interpretation ◽  
Realistic Model ◽  
High Energy ◽  
Starburst Galaxies ◽  
Neutrino Factory ◽  
High Energy Cosmic Rays ◽  
Astrophysical Objects

ABSTRACT Starburst galaxies, which are known as ‘reservoirs’ of high-energy cosmic-rays, can represent an important high-energy neutrino ‘factory’ contributing to the diffuse neutrino flux observed by IceCube. In this paper, we revisit the constraints affecting the neutrino and gamma-ray hadronuclear emissions from this class of astrophysical objects. In particular, we go beyond the standard prototype-based approach leading to a simple power-law neutrino flux, and investigate a more realistic model based on a data-driven blending of spectral indexes, thereby capturing the observed changes in the properties of individual emitters. We then perform a multi-messenger analysis considering the extragalactic gamma-ray background (EGB) measured by Fermi-LAT and different IceCube data samples: the 7.5-yr high-energy starting events (HESE) and the 6-yr high-energy cascade data. Along with starburst galaxies, we take into account the contributions from blazars and radio galaxies as well as the secondary gamma-rays from electromagnetic cascades. Remarkably, we find that, differently from the highly-constrained prototype scenario, the spectral index blending allows starburst galaxies to account for up to $40{{\ \rm per\ cent}}$ of the HESE events at $95.4{{\ \rm per\ cent}}$ CL, while satisfying the limit on the non-blazar EGB component. Moreover, values of $\mathcal {O}(100\, \mathrm{PeV})$ for the maximal energy of accelerated cosmic-rays by supernovae remnants inside the starburst are disfavoured in our scenario. In broad terms, our analysis points out that a better modelling of astrophysical sources could alleviate the tension between neutrino and gamma-ray data interpretation.

Experimentally guided Monte Carlo calculations of the atmospheric muon and neutrino flux

2006 ◽  
Vol 151 (1) ◽  
pp. 295-298 ◽  
Author(s):  
B. Mitrica ◽  
I.M. Brancus ◽  
H. Rebel ◽  
J. Wentz ◽  
A. Bercuci ◽  
...  
Keyword(s):  
Monte Carlo ◽  
Neutrino Flux ◽  
Monte Carlo Calculations ◽  
Atmospheric Muon
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