Scintillator-based transition radiation detectors for very high-energy particles

2004 ◽  
Vol 522 (1-2) ◽  
pp. 73-76 ◽  
Author(s):  
Michael L. Cherry ◽  
Gary L. Case
Keyword(s):  
Transition Radiation ◽  
Radiation Detectors ◽  
High Energy ◽  
Very High Energy ◽  
High Energy Particles ◽  
Very High

scholarly journals Plasma Energetics in Solar Flares

1980 ◽  
Vol 5 ◽  
pp. 343-350 ◽  
Author(s):  
Gerard Van Hoven
Keyword(s):  
Gamma Rays ◽  
Solar Flares ◽  
High Energy ◽  
Physical Mechanisms ◽  
Very High Energy ◽  
Physical Effects ◽  
High Energy Particles ◽  
The Magnetic Field ◽  
Dissipation Processes ◽  
Very High

I want to begin with the observation, which I will try to make clear in the following, that a solar flare comprises an incredibly complex set of phenomena. This is not only true with respect to what is seen and measured in spectacular examples, but also when one considers the constituent parts of simple, even idealized, cases. A series of different physical effects lead, as one illustration, to radiations from the flare-instability site and its surroundings which span the range from meter waves to gamma rays (Svestka 1976, Sturrock 1979).To fit within the context of this discussion, I will concentrate on the high-temperature and quasi-thermal aspects of a flare, and on the basic physical mechanisms connected with the primary energization and dissipation processes. Thus, I will treat the reconnection of the magnetic field, the bulk acceleration of particles, the thermalization and the ultimate radiation of the energy. I will not treat the optical manifestations or, at the other extreme, the acceleration of very high energy particles.

scholarly journals Optical Inverse Compton Emission in Extragalactic Radio Sources

1982 ◽  
Vol 97 ◽  
pp. 71-73
Author(s):  
S. E. Okoye ◽  
O. Obinabo
Keyword(s):  
Radio Source ◽  
Optical Emission ◽  
Structural Data ◽  
High Energy ◽  
Radio Sources ◽  
Inverse Compton ◽  
Source Component ◽  
Very High Energy ◽  
High Energy Particles ◽  
Very High

In this contribution the reported detection by Saslaw, Tyson and Crane (1978) of weak optical emission in the lobes of three 3C sources — 3C 265, 3C 285 and 3C 390.3 — is reappraised in the framework of three optical emission mechanisms — synchrotron (SYN), synchrotron inverse Compton (SIC) and blackbody inverse Compton (BIC). This effort has been motivated partly by the knowledge that the contribution to the synchrotron inverse Compton emission in a radio source component is likely to become significant for very compact and bright radio components (see e.g. Okoye 1972), and partly by the recent availability of high resolution radio frequency structural data on the sources in question. Another incentive arose from the demands of a separate investigation into high energy particles interactions in radio sources (reported by Okoye and Okeke in this volume) involving very high energy protons thus making it necessary to ascertain whether such highly energetic particles exist in radio source components.

Particle Acceleration by Pulsars

1981 ◽  
Vol 94 ◽  
pp. 175-204 ◽  
Author(s):  
Jonathan Arons
Keyword(s):  
High Energy ◽  
Rotational Energy ◽  
Pair Creation ◽  
X Ray ◽  
Current State ◽  
Very High Energy ◽  
Γ Ray ◽  
High Energy Particles ◽  
Relativistic Particles ◽  
Very High

The evidence that pulsars accelerate relativistic particles is reviewed, with emphasis on the γ-ray observations. The current state of knowledge of acceleration in strong waves is summarized, with emphasis on the inability of consistent theories to accelerate very high energy particles without converting too much energy into high energy photons. The state of viable models for pair creation by pulsars is summarized, with the conclusion that pulsars very likely lose rotational energy in winds instead of in superluminous strong waves. The relation of the pair creation models to γ-ray observations and to soft X-ray observations of pulsars is outlined, with the conclusion that energetically viable models may exist, but none have yet yielded useful agreement with the extant data. Some paths for overcoming present problems are discussed.

Strong interactions at very high energy

1964 ◽  
Vol 82 (1) ◽  
pp. 3-81 ◽  
Author(s):  
Evgenii L. Feinberg ◽  
Dmitrii S. Chernavskii
Keyword(s):  
High Energy ◽  
Strong Interactions ◽  
Very High Energy ◽  
Very High
Sign in / Sign up

Export Citation Format

Share Document