scholarly journals Cosmic ray acceleration to very high energy through the non-linear amplification by cosmic rays of the seed magnetic field

2001 ◽  
Vol 321 (3) ◽  
pp. 433-438 ◽  
Author(s):  
A. R. Bell ◽  
S. G. Lucek
Keyword(s):  
Magnetic Field ◽  
Cosmic Rays ◽  
Cosmic Ray ◽  
High Energy ◽  
Linear Amplification ◽  
Cosmic Ray Acceleration ◽  
Non Linear ◽  
Very High Energy ◽  
Very High

scholarly journals Gamma-Ray Bursts at TeV Energies: Observational Status

Galaxies ◽  
2022 ◽  
Vol 10 (1) ◽  
pp. 7
Author(s):  
Koji Noda ◽  
Robert Daniel Parsons
Keyword(s):  
Gamma Ray ◽  
Cosmic Ray ◽  
High Energy ◽  
Gamma Ray Bursts ◽  
High Energy Gamma ◽  
Cosmic Ray Acceleration ◽  
Very High Energy ◽  
Energy Gamma ◽  
Observational Status ◽  
Very High

Gamma-ray bursts (GRBs) are some of the most energetic events in the Universe and are potential sites of cosmic ray acceleration up to the highest energies. GRBs have therefore been a target of interest for very high energy gamma-ray observatories for many years, leading to the recent discovery of a number of bursts with photons reaching energies above 100 GeV. We summarize the GRB observational campaigns of the current generation of very high energy gamma-ray observatories as well as describing the observations and properties of the GRBs discovered so far. We compare the properties of the very high energy bursts to the total GRB distribution and make predictions for the next generation of very high energy gamma-ray observations.

scholarly journals Opening Remarks ~ Prospects of very high energy cosmic ray interactions for astroparticle physics

2019 ◽  
Vol 208 ◽  
pp. 01001
Author(s):  
Yoshitaka Itow
Keyword(s):  
Cosmic Rays ◽  
Particle Production ◽  
Cosmic Ray ◽  
High Energy ◽  
Hadronic Interactions ◽  
High Energy Cosmic Rays ◽  
Cosmic Ray Interactions ◽  
Precise Knowledge ◽  
Very High Energy ◽  
Very High

Hadronic interactions of very high energy cosmic rays have been studied in various aspects of motivation. In recent decades, mainly motivated by air shower experiments, modelling of very high energy cosmic ray interactions have been greatly improved together with new data obtained from high energy colliders such as the LHC. Regarding recent rapid progress of multi-messenger astronomy, a precise knowledge on secondary particle production by cosmic rays at very high energy is largely indispensable. This would give us a new insight and new motivation to study minimum bias hadronic interactions of very high energy cosmic rays.

scholarly journals Time-dependent escape of cosmic rays from supernova remnants potentially at the origin of the very-high-energy cosmic-ray gradient of the Galactic center

2020 ◽  
Vol 644 ◽  
pp. A113
Author(s):  
L. Jouvin ◽  
A. Lemière ◽  
R. Terrier
Keyword(s):  
Cosmic Rays ◽  
Supernova Remnants ◽  
Galactic Center ◽  
Large Fraction ◽  
Surrounding Medium ◽  
Cosmic Ray ◽  
High Energy ◽  
Very High Energy ◽  
Energy Dependent ◽  
Very High

The distribution of the very-high-energy diffuse emission in the inner 200 pc measured by H.E.S.S. indicates the existence of a pronounced cosmic-ray (CR) gradient peaking on the Galactic center (GC). Previous studies have shown that these data are consistent with a scenario in which the CRs are diffused away from a stationary source at the GC. We previously showed that, taking the 3D gas distribution and a realistic distribution of supernova explosions into account, CRs accelerated in supernova remnants should account for a large fraction of the GC CRs observed by H.E.S.S.; but the model did not fully reproduce the apparent over-density in the inner 30 pc. In this work, we study the time-energy dependent cosmic rays escape from the remnant that is expected to occur when the shock wave decelerates in the surrounding medium. We show that the resulting CR distribution follows the quasi-stationary profile observed by H.E.S.S. more closely. The main signature is that the energy-dependent escape creates a strong dependency of the morphology of the γ-ray emission with the energy. The existence of this energy dependency should be observable by the Cherenkov Telescope Array.

scholarly journals Ultra-high-energy cosmic ray acceleration by magnetic reconnection in relativistic jets and the origin of very high energy emission

2021 ◽  
Author(s):  
Elisabete De Gouveia Dal Pino ◽  
Tania E. Medina-Torrejon ◽  
Luis H.S. Kadowaki ◽  
Grzergoz Kowal ◽  
Juan Carlos Rodriguez-Ramirez
Keyword(s):  
Magnetic Reconnection ◽  
Cosmic Ray ◽  
High Energy ◽  
Ultra High Energy ◽  
Relativistic Jets ◽  
Energy Emission ◽  
Cosmic Ray Acceleration ◽  
Very High Energy ◽  
High Energy Emission ◽  
Very High

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.

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