Hostname: page-component-848d4c4894-x5gtn Total loading time: 0 Render date: 2024-05-22T02:42:51.894Z Has data issue: false hasContentIssue false
  • English
  • Français

Results of two balloon flights for the detection of high energy γ-rays

Published online by Cambridge University Press:  14 August 2015

M. Niel ,
G. Vedrenne  and
R. Bouigue
M. Niel
Affiliation:
Centre d'Etude Spatiale des Rayonnements
G. Vedrenne
Affiliation:
Centre d'Etude Spatiale des Rayonnements
R. Bouigue
Affiliation:
Observatoire de Toulouse

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

After many years of fruitless research on primary γ-Rays, the results obtained by Clark et al. [1] with the OSO-3 satellite, proved for the first time the existence of a primary γ-Ray flux. The study of the distribution of this radiation showed a strong anisotropy in the direction of the galactic disk and, more precisely, in the direction of the galactic center. Now the production of γ-Rays in the spatial medium is related to high energy processes and to the presence of relativistic electrons. The high energy processes bring about an emission of γ-Rays essentially by decay of the π° mesons created for instance, by the interaction of cosmic radiation with interstellar matter or by matter-antimatter annihilation. The relativistic electrons can lead to an emission of γ-Rays by various processes: in particular, by bremsstrahlung of the electrons in the interstellar matter or by the Inverse Compton effect with the photons of the stellar light or of the infrared radiation background.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 37: Non-Solar X- and Gamma-Ray Astronomy , 1970 , pp. 325 - 334
Copyright
Copyright © Reidel 1970 

References

[1] Clark, G. W., Garmire, G. P., and Kraushaar, W. L.: 1968, Astrophys. J. Letters 153, L 203.CrossRefGoogle Scholar
[2] Ginzburg, V. L. and Syrovatsky, S. I.: 1964, Origin of Cosmic Rays.Google Scholar
[3] Garmire, G. and Kraushaar, W. L.: 1965, Space Sci. Rev. 4, 123.CrossRefGoogle Scholar
[4] Gould, R. J. and Burbidge, G. R.: 1966, Handbuch der Physik 46, No. 2.Google Scholar
[5] Fazio, G. G.: 1967, Ann. Rev. Astron. Astrophys. 5, 481.CrossRefGoogle Scholar
[6] Stecker, F. W.: 1969, Nature 222, 865.CrossRefGoogle Scholar
[7] Ögelman, H.: 1969, Nature 221, 753.Google Scholar
[8] Niel, M., Cassignol, M., Vedrenne, G., and Bouigue, R.: 1969, Nucl. Instr. Methods. 69, 309.Google Scholar
[9] Cline, T. L.: 1961, Phys. Rev. Letters. 7, 109.Google Scholar
[10] Duthie, J. G., Cobb, R., and Stewart, J.: 1966, Phys. Rev. Letters 17, 263.Google Scholar
[11] Fichtel, C. E., Kniffen, D. A., Ögelman, H. B.: COSPAR 69 (Rome), to be published.Google Scholar
[12] Olsen, H.: 1963, Phys. Rev. 131, 406.Google Scholar
[13] Stecker, F. W.: 1968, Nasa TMX 63 181, April.Google Scholar
[14] Fazio, G. G., Helmken, H. F., Cavrak, S. J., and Hearn, D. R.: 1968, Can. J. Phys. 46, S427.Google Scholar
[15] Fichtel, C. E., Kniffen, D. A., and Ögelman, H. B.: 1968, NASA Report X 611, 69 58, February.Google Scholar
[16] Hearn, D.: 1969, Nucl. Instr. Methods 70, 200.Google Scholar