Synchrotron Radiation III—High Energies

2019 ◽  
pp. 417-426
Author(s):  
Julian Schwinger ◽  
Lester L. DeRaad ◽  
Kimball A. Milton ◽  
Wu-yang Tsai
2021 ◽  
Vol 914 (2) ◽  
pp. 76
Author(s):  
Dmitry Khangulyan ◽  
Felix Aharonian ◽  
Carlo Romoli ◽  
Andrew Taylor

2010 ◽  
Vol 6 (S272) ◽  
pp. 638-639 ◽  
Author(s):  
Delia Volpi ◽  
Ronny Blomme ◽  
Michael De Becker ◽  
Gregor Rauw

AbstractSome OB stars show variable non-thermal radio emission. The non-thermal emission is due to synchrotron radiation that is emitted by electrons accelerated to high energies. The electron acceleration occurs at strong shocks created by the collision of radiatively-driven stellar winds in binary systems. Here we present results of our modelling of two colliding wind systems: Cyg OB2 No. 8A and Cyg OB2 No. 9.


Author(s):  
A. Howie ◽  
D.W. McComb

The bulk loss function Im(-l/ε (ω)), a well established tool for the interpretation of valence loss spectra, is being progressively adapted to the wide variety of inhomogeneous samples of interest to the electron microscopist. Proportionality between n, the local valence electron density, and ε-1 (Sellmeyer's equation) has sometimes been assumed but may not be valid even in homogeneous samples. Figs. 1 and 2 show the experimentally measured bulk loss functions for three pure silicates of different specific gravity ρ - quartz (ρ = 2.66), coesite (ρ = 2.93) and a zeolite (ρ = 1.79). Clearly, despite the substantial differences in density, the shift of the prominent loss peak is very small and far less than that predicted by scaling e for quartz with Sellmeyer's equation or even the somewhat smaller shift given by the Clausius-Mossotti (CM) relation which assumes proportionality between n (or ρ in this case) and (ε - 1)/(ε + 2). Both theories overestimate the rise in the peak height for coesite and underestimate the increase at high energies.


Author(s):  
B. Jouffrey ◽  
D. Dorignac ◽  
A. Bourret

Since the early works on GP zones and the model independently proposed by Preston and Guinier on the first steps of precipitation in supersaturated solid solution of aluminium containing a few percent of copper, many works have been performed to understand the structure of different stages in the sequence of precipitation.The scheme which is generally admitted can be drawn from a work by Phillips.In their original model Guinier and Preston analysed a GP zone as composed of a single (100) copperrich plane surrounded by aluminum atomic planes with a slightly shorter distance from the original plane than in the solid solution.From X-ray measurements it has also been shown that GP1 zones were not only copper monolayer zones. They could be up to a few atomic planes thick. Different models were proposed by Guinier, Gerold, Toman. Using synchrotron radiation, proposals have been recently made.


2001 ◽  
Vol 16 (1-2) ◽  
pp. 49-85
Author(s):  
A. De Roeck

2005 ◽  
Vol 25 (1_suppl) ◽  
pp. S558-S558
Author(s):  
Masahiro Tamaki ◽  
Takashi Mizobe ◽  
Keiji Kidoguchi ◽  
Junnji Koyama ◽  
Takeshi Kondoh ◽  
...  

1973 ◽  
Vol 34 (C8) ◽  
pp. C8-63-C8-63
Author(s):  
J. BARRINGTON LEIGH ◽  
G. ROSENBAUM

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