scholarly journals Earth-Skimming Ultrahigh Energy Tau Neutrinos Simulated with Monte Carlo Method and CONEX Code

2021 ◽  
Vol 2021 ◽  
pp. 1-7
Author(s):  
Bouzid Boussaha ◽  
Tariq Bitam
Keyword(s):  
Monte Carlo ◽  
Cosmic Ray ◽  
High Energy ◽  
Tau Lepton ◽  
Ultrahigh Energy ◽  
Air Shower ◽  
Mountain Valley ◽  
Tau Neutrinos ◽  
Very High Energy ◽  
Very High

This paper is aimed at studying the feasibility of building an Earth-skimming cosmic tau neutrinos detector, with the aim of eventually identifying the ideal dimensions of a natural site mountain-valley for the detection of very high energy neutrinos tau range from 1 0 16 eV to 1 0 20 eV , as well as possibly locate one such site in Algeria. First, a Monte Carlo simulation of the neutrino-[mountain] matter interaction as well as the resulting decay of the tau lepton is conducted to determine the optimal dimensions of the mountain as well as the location of the tau decay in the valley. Second, a CORSIKA (COsmic Ray Simulation for KAscade) simulation with the CONEX option is conducted to track the evolution of the almost horizontal air shower initiated by the tau lepton. Many particles are produced, which are part of the shower components: electrons, muons, gammas, pions, etc. The study of the spatial distribution of these particles enables the discovery of the optimal width of the valley, and consequently, the distance at which to lay the detection network.

scholarly journals Comparison of the Measurement and Simulation with KM2A Prototype Array

2019 ◽  
Vol 208 ◽  
pp. 14006
Author(s):  
Zhe Li ◽  
Songzhan Chen ◽  
Huihai He ◽  
Cong Li ◽  
Hongkui Lv ◽  
...  
Keyword(s):  
Gamma Ray ◽  
Cosmic Ray ◽  
High Energy ◽  
Stable Operation ◽  
Air Shower ◽  
Very High Energy ◽  
Energy Gamma ◽  
Many Sources ◽  
Very High ◽  
Monte Carlo Simulation Program

The Large High Altitude Air Shower Observatory (LHAASO) is a new hybrid array for very high energy gamma ray astronomy and cosmic ray physics. The KM2A array, one of the main parts of LHAASO, covers an area of 1.3 km2 to observe gamma rays above 10 TeV up to 1 PeV for many sources. A prototype with 1% the size of the whole KM2A has been in stable operation for more than two years. A Monte Carlo simulation program named G4KM2A was developed; based on this work, the trigger rate, hit multiplicity, angular and core reconstruction are compared with KM2A prototype data. Finally, the moon shadow with -6.5 significance was obtained. The G4KM2A simulation results are consistent with KM2A prototype data and can be used for the whole KM2A array in future.

scholarly journals TRACING VERY HIGH ENERGY TAU NEUTRINOS FROM COSMOLOGICAL SOURCES IN ICE

2005 ◽  
Vol 20 (06) ◽  
pp. 1204-1211 ◽  
Author(s):  
J. JONES ◽  
I. MOCIOIU ◽  
I. SARCEVIC ◽  
M. H. RENO
Keyword(s):  
High Energy ◽  
Ultrahigh Energy ◽  
Tau Neutrino ◽  
Tau Neutrinos ◽  
The Earth ◽  
Very High Energy ◽  
Charged Leptons ◽  
Neutrino Fluxes ◽  
In Transit ◽  
Very High

Astrophysical sources of ultrahigh energy neutrinos yield tau neutrino fluxes due to neutrino oscillations. We study in detail the contribution of tau neutrinos with energies above 106 GeV relative to the contribution of the other flavors. We consider several different initial neutrino fluxes and include tau neutrino regeneration in transit through the Earth and energy loss of charged leptons. We discuss signals of tau neutrinos in detectors such as IceCube, RICE and ANITA.

scholarly journals HOMAGE TO PROFESSOR OSCAR SAAVEDRA SAN MARTIN

2019 ◽  
Vol 208 ◽  
pp. 10002
Author(s):  
E.H. SHIBUYA
Keyword(s):  
Special Section ◽  
Cosmic Ray ◽  
High Energy ◽  
Emeritus Professor ◽  
High Energy Cosmic Rays ◽  
Air Shower ◽  
Very High Energy ◽  
San Martín ◽  
Very High ◽  
Joint Experiment

Professor Oscar Saavedra San Martin passed away on 8 April 2018 at Bonvicino-Italy. The Organizing Committee of the 20th International Symposium on Very High Energy Cosmic Rays-ISVHECRI-2018, held in Nagoya, Japan decided to pay a tribute to Oscar, born on 29 June, 1940 at LaPaz, Bolivia. During the banquet, a small presentation in honour to Oscar was scheduled in a special section of Wednesday 23 May 2018. His last participation was at the 19th ISVHECRI held in Moscow, Russian Federation, during the period 22-27 August 2016. Oscar joined the BASJE-Bolivian Air Shower Joint Experiment in 1966, a collaboration between Bolivia and Japan. The aim of BASJE was to search for high energy γ's coming mainly from the center of Galaxy, due to the Chacaltaya location. From 1967 to 1968 he served as Director of the Cosmic Ray Laboratory at Chacaltaya following the BASJE experiments. Due to his huge contribution to Bolivian Science, Oscar received in 2009 the Doctor Honoris Causa title and was nominated Scientific Ambassador of his motherland. He gained his Doctorate from Milan University in 1964 and after immigration to Italy was a staff member of Torino University. On his retirement Torino University awarded him the title of Emeritus Professor.

scholarly journals Recent Results from the CANGAROO Project

1996 ◽  
Vol 160 ◽  
pp. 363-364
Author(s):  
S.A. Dazeley ◽  
P.G. Edwards ◽  
J.R. Patterson ◽  
G.P. Rowell ◽  
M. Sinnott ◽  
...  
Keyword(s):  
Gamma Rays ◽  
South Australia ◽  
Cosmic Ray ◽  
High Energy ◽  
Relativistic Electrons ◽  
Large Numbers ◽  
Inverse Compton ◽  
Very High Energy ◽  
Large Telescopes ◽  
Very High

TheCollaboration ofAustralia andNippon for aGAmmaRayObservatory in theOutback operates two large telescopes at Woomera (South Australia), which detect the Čerenkov light images produced in the atmosphere by electronpositron cascades initiated by very high energy (~1 TeV or 1012eV) gamma rays. These gamma rays arise from a different mechanism than at EGRET energies: inverse Compton (IC) emission from relativistic electrons.The spoke-like images are recorded by a multi-pixel camera which facilitates the rejection of the large numbers of oblique and ragged cosmic ray images. A field of view ~3.5° is required. The Australian team operates a triple 4 m diameter mirror telescope, BIGRAT, with a 37 photomultiplier tube camera and energy threshold 600 GeV. The Japanese operate a single, highly accurate 3.8 m diameter f/1 telescope and high resolution 256 photomultipler tube camera. In 1998 a new 7 m telescope is planned for Woomera with a design threshold ~;200GeV.

scholarly journals High Energy γ-Rays from the Direction of the Crab Pulsar

1981 ◽  
Vol 94 ◽  
pp. 327-328
Author(s):  
T. Dzikowski ◽  
B. Grochalska ◽  
J. Gawin ◽  
J. Wdowczyk
Keyword(s):  
High Energy ◽  
Crab Pulsar ◽  
Muon Detector ◽  
Extensive Air Shower ◽  
Air Shower ◽  
Very High Energy ◽  
Γ Rays ◽  
Shower Array ◽  
Very High ◽  
Air Shower Array

A search has been made for very high energy photons from the direction of the Crab Pulsar using the Lodz extensive air shower array. This device is particularly suitable for such a study because it consists of a large muon detector which can be used to search for the characteristic muon poor showers.

scholarly journals Neutrino and γ-ray Emission from the Core of NGC1275 by Magnetic Reconnection: GRMHD Simulations and Radiative Transfer/Particle Calculations

2018 ◽  
Vol 14 (S342) ◽  
pp. 184-188
Author(s):  
J. C. Rodríguez-Ramírez ◽  
Elisabete M. de Gouveia Dal Pino ◽  
R. Alves Batista
Keyword(s):  
Monte Carlo ◽  
Radiative Transfer ◽  
Magnetic Reconnection ◽  
Neutrino Flux ◽  
Cosmic Ray ◽  
High Energy ◽  
Emission Model ◽  
The Core ◽  
Very High Energy ◽  
General Relativistic

AbstractVery high energy (VHE) emission has been detected from the radio galaxy NGC1275, establishing it as a potential cosmic-ray (CR) accelerator and a high energy neutrino source. We here study neutrino and γ-ray emission from the core of NGC1275 simulating the interactions of CRs assumed to be accelerated by magnetic reconnection, with the accreting plasma environment. To do this, we combine (i) numerical general relativistic (GR) magneto-hydrodynamics (MHD), (ii) Monte Carlo GR leptonic radiative transfer and, (iii) Monte Carlo interaction of CRs. A leptonic emission model that reproduces the SED in the [103-1010.5] eV energy range is used as the background target for photo-pion interactions+electromagnetic cascading. CRs injected with the power-law index κ=1.3 produce an emission profile that matches the VHE tail of NGC1275. The associated neutrino flux, below the IceCube limits, peaks at ∼PeV energies. However, coming from a single source, this neutrino flux may be an over-estimation.

Sign in / Sign up

Export Citation Format

Share Document