Vavilov–Cherenkov radiation when cosmic rays pass through the relic photon gas and when fast charged particles traverse an optical laser beam

2016 ◽  
Vol 123 (1) ◽  
pp. 12-16 ◽  
Author(s):  
S. G. Chefranov
Keyword(s):  
Cosmic Rays ◽  
Laser Beam ◽  
Cherenkov Radiation ◽  
Charged Particles ◽  
Photon Gas ◽  
Pass Through ◽  
Optical Laser

Oliver Heaviside: an accidental time traveller

2018 ◽  
Vol 376 (2134) ◽  
pp. 20170448
Author(s):  
Paul J. Nahin
Keyword(s):  
Cherenkov Radiation ◽  
Charged Particles ◽  
Electromagnetic Theory ◽  
Time Travel ◽  
Characteristic Radiation ◽  
Theme Issue ◽  
The Past ◽  
Faster Than Light

A little discussed aspect of Heaviside's work in electromagnetics concerned faster-than-light (FTL) charged particles, precursors to the hypothetical tachyon and his discovery that such motion should produce a characteristic radiation signature (now called Cherenkov radiation ). When Heaviside wrote, the time travel implications of FTL were not known (Einstein was still a teenager), and in this paper some speculations are offered on what Heaviside would have thought of FTL time travel, and of the associated (now classic) time travel paradoxes, including the possibility (or not) of sending information into the past. This article is part of the theme issue ‘Celebrating 125 years of Oliver Heaviside's ‘Electromagnetic Theory’’.

ENERGY ORDERING EFFECTS IN THE ARRIVAL DIRECTIONS OF ULTRA-HIGH ENERGY COSMIC RAYS MEASURED BY THE PIERRE AUGER OBSERVATORY

2011 ◽  
Vol 20 (supp02) ◽  
pp. 50-56
Author(s):  
◽  
PETER SCHIFFER
Keyword(s):  
Cosmic Rays ◽  
Magnetic Fields ◽  
Charged Particles ◽  
High Energy ◽  
Pierre Auger Observatory ◽  
Ultra High Energy ◽  
High Energy Cosmic Rays ◽  
Ordering Effects ◽  
Arrival Directions

The Pierre Auger Observatory is the world's largest experiment for the measurement of ultra-high energy cosmic rays (UHECRs). These UHECRs are assumed to be to be charged particles, and thus are deflected in cosmic magnetic fields. Recent results of the Pierre Auger Observatory addressing the complex of energy ordering of the UHECRs arrival directions are reviewed in this contribution. So far no significant energy ordering has been observed.

scholarly journals INFLUENCE OF PRIMARY COSMIC RADIATION MASS COMPOSITION ON THE ESTIMATION OF EAS ENERGY

2005 ◽  
Vol 20 (29) ◽  
pp. 6897-6899 ◽  
Author(s):  
S. P. KNURENKO ◽  
A. A. IVANOV ◽  
V. A. KOLOSOV ◽  
Z. E. PETROV ◽  
I. YE. SLEPTSOV ◽  
...  
Keyword(s):  
Cosmic Radiation ◽  
Cherenkov Radiation ◽  
Charged Particles ◽  
Mass Composition ◽  
Mixed Composition ◽  
Radiation Data ◽  
Primary Particles ◽  
Primary Cosmic Radiation ◽  
Electron Photon ◽  
Photon Component

Fraction of energy, E em /E0, transferred to the electron-photon component of EAS at E0 = 1015 ± 1019 eV was estimated by using the Cherenkov radiation data and the data on charged particles obtained at the Yakutsk EAS array. The results are compared with predictions of different models for energy dissipation into the EAS electron-photon component and with calculations performed with different primary nuclei content. In the energy ranges 1015 ± 1016 eV and 1018 ± 1019 eV , the ratio E em /E0 is equal to (77 ± 2)% and (88 ± 2)%, respectively, that does not contradict to a mixed composition of primary particles in the first energy interval and purely proton composition in the second one.

scholarly journals KM3NeT acoustic positioning and detection system

2019 ◽  
Vol 216 ◽  
pp. 02006 ◽  
Author(s):  
Salvatore Viola
Keyword(s):  
Cherenkov Radiation ◽  
Detection System ◽  
Charged Particles ◽  
Positioning System ◽  
Atmospheric Neutrinos ◽  
Neutrino Telescopes ◽  
Strongly Connected ◽  
Radiation Induced ◽  
Better Than ◽  
Acoustic Positioning

In the Mediterranean Sea, the KM3NeT Collaboration is constructing a the deep-sea research infrastructure hosting next generation neutrino telescopes. In the KM3NeT telescopes the Cherenkov radiation induced by the secondary charged particles produced in the interaction of cosmic and atmospheric neutrinos within an effective volume between megaton and several cubic kilometers of water are detected by an array of thousands of photomultipliers. The capability of the telescope to determine the direction of secondary charged particles and to point back to the neutrino source is strongly connected to the accuracy on photomultipliers positions. In KM3NeT, the photomultiplier positions are continuously monitored by an acoustic positioning system, designed by the KM3NeT Collaboration to reach an accuracy of the photomultiplier positions better than 20 cm.

scholarly journals Conical Interfaces between Two Immiscible Fluids Induced by an Optical Laser Beam

2019 ◽  
Vol 122 (17) ◽  
Author(s):  
A. Girot ◽  
J. Petit ◽  
R. Saiseau ◽  
T. Guérin ◽  
H. Chraibi ◽  
...  
Keyword(s):  
Laser Beam ◽  
Immiscible Fluids ◽  
Optical Laser

scholarly journals 5. Study of Cosmic Rays by Rockets and Sputniks in the U.S.S.R.

1960 ◽  
Vol 10 ◽  
pp. 710-712
Author(s):  
S. N. Vernov ◽  
A. E. Chudakov
Keyword(s):  
Cosmic Rays ◽  
Charged Particles ◽  
Light Elements ◽  
Primary Particles ◽  
In The Beginning ◽  
Electron Photon ◽  
Photon Component

In the U.S.S.R. the study of cosmic rays by rockets was started in 1947.In the beginning, with the help of Geiger counters the number of charged particles was measured, and the formation of the electron-photon component in the interaction of primary particles of cosmic rays with nuclei of light elements was investigated.

The interaction of pulsar winds with old supernova remnants

2000 ◽  
Vol 177 ◽  
pp. 513-514
Author(s):  
Eric van der Swaluw ◽  
Abraham Achterberg ◽  
Yves A. Gallant
Keyword(s):  
Cosmic Rays ◽  
Shock Waves ◽  
Radio Emission ◽  
Supernova Remnants ◽  
Charged Particles ◽  
Simple Problem ◽  
Relativistic Electrons ◽  
First Case ◽  
Pulsar Wind ◽  
Pulsar Winds

Shock waves in young supernova remnants (SNR) are generally considered to be the places where production and acceleration of charged particles (relativistic electrons and cosmic rays) take place. Older remnants can be re-energised if an active pulsar catches up with the shell of the remnant (Shull, Fesen, & Saken 1989). In that case a pulsar-driven wind can inject energetic particles into the shell, resulting into a rejuvenation of the radio emission of the old remnant due to the presence of additional relativistic electrons.Radio observations of CTB80 (Angerhofer et al. 1981) and G5.4-1.2 (Frail & Kulkarni 1991) give evidence for the importance of the presence of an active pulsar close to the old shell of the remnants. In the first case the pulsar is believed to be inside the SNR. In the second case the pulsar is thought to have penetrated the shell of the SNR, and resides in the interstellar medium (ISM). We intend to investigate the physics which are connected with these kind of systems. One expects new effects resulting from the interaction of the three different shocks; the SNR shock, the bowshock bounding the pulsar wind nebula (PWN) and the (pulsar) wind termination shock. The dynamics of the system is described by a hydrodynamics code. We use the results from the hydrodynamics code to investigate the process of acceleration and transport of particles which are advected by the flow and diffuse with respect to the flow. We have applied the latter to a simple problem, the case of a spherically expanding SNR.

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