Hostname: page-component-cd9895bd7-gbm5v Total loading time: 0 Render date: 2024-12-26T03:24:13.307Z Has data issue: false hasContentIssue false
  • English
  • Français

Fast Electrons in Small Solar Flares

Published online by Cambridge University Press:  14 August 2015

R. P. Lin
R. P. Lin*
Affiliation:
Space Sciences Laboratory, University of California, Berkeley, Calif. 94720, U.S.A.

Abstract

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.

Because ∼5–100 keV electrons are frequently accelerated and emitted by the Sun in small flares, it is possible to define a detailed characteristic physical picture of these events. This review summarizes both the direct spacecraft observations of non-relativistic solar electrons, and observations of the X-ray and radio emission generated by these particles at the Sun and in the interplanetary medium. These observations bear on the basic astrophysical process of particle acceleration in tenuous plasmas. We find that in many small solar flares the ∼5–100 keV electrons accelerated during flash phase constitute the bulk of the total flare energy. Thus the basic flare mechanism in these flares essentially converts the available flare energy into fast electrons. These electrons may produce the other flare electromagnetic emissions through their interactions with the solar atmosphere. In large proton flares these electrons may provide the energy to eject material from the Sun and to create a shock wave which could then accelerate nuclei and electrons to much higher energies.

Type
Part 3: Solar Flares
Information
Symposium - International Astronomical Union , Volume 68: Solar X, Gamma, and EUV Radiation , 1975 , pp. 385 - 409
Copyright
Copyright © Reidel 1975 

References

Anderson, K. A. and Lin, R. P.: 1966, Phys. Rev. Letters 16, 1121.Google Scholar
Anderson, K. A. and Winckler, J. R.: 1962, J. Geophys. Res. 67, 4103.Google Scholar
Arnoldy, R. L., Kane, S. R., and Winckler, J. R.: 1968, Astrophys. J. 151, 711.Google Scholar
Berger, M. J. and Seltzer, S. M.: 1964, ‘Tables of Energy Losses and Ranges of Electrons and Positrons’, NASA SP-3012.Google Scholar
Brown, J. C.: 1971, Solar Phys. 18, 450.Google Scholar
Brown, J. C.: 1972, Solar Phys. 25, 158.Google Scholar
Datlowe, D.: 1975, This volume, p. 191.Google Scholar
Datlowe, D. and Lin, R. P.: 1973, Solar Phys. 32, 459.Google Scholar
Fainberg, J., Evans, L. G., and Stone, R. G.: 1972, Science 178, 743.Google Scholar
Hamberger, S. M., Jancarik, J., Sharp, L. E., Aldcroft, D. A., and Wetherall, A.: 1971, Proc. International Conference Plasma Physics and Controlled Nuclear Fusion, Vol. II, 37.Google Scholar
Holt, S. S. and Ramaty, R.: 1969, Solar Phys. 8, 119.Google Scholar
Hoyng, P., Brown, J. C., Stevens, G., and Van Beek, H. E.: 1975, This volume, p. 233.Google Scholar
Hudson, H. S.: 1972, Solar Phys. 24, 414.Google Scholar
Hudson, H. S., Jones, T. W., and Lin, R. P.: 1975, This volume, p. 425.CrossRefGoogle Scholar
Hudson, H. S., Peterson, L. E., and Schwartz, D. A.: 1969, Astrophys. J. 157, 389.Google Scholar
Hundhausen, A. J.: 1972, in Sonett, C. P., Coleman, P. J. Jr., and Wilcox, J. M. (eds.), Solar Wind, NASA SP-308, p. 393.Google Scholar
Jackson, J. D.: 1962, Classical Electrodynamics, J. Wiley and Sons, New York.Google Scholar
Kahler, S. W. and Kreplin, R. W.: 1971, Astrophys. J. 168, 531.CrossRefGoogle Scholar
Kahler, S. W., Meekins, J. F., Kreplin, R. W., and Bowyer, C. S.: 1970, Astrophys. J. 162, 293.CrossRefGoogle Scholar
Kane, S. R.: 1971, Astrophys. J. 170, 587.Google Scholar
Kane, S. R.: 1972, Solar Phys. 27, 174.Google Scholar
Kane, S. R.: 1973a, Bull. A.A.S. 5, 274.Google Scholar
Kane, S. R.: 1973b, in Ramaty, R. and Stone, R. G. (eds.), High Energy Phenomena on the Sun, NASA SP-342, p. 55.Google Scholar
Kane, S. R.: 1974, Private communication.Google Scholar
Kane, S. R. and Anderson, K. A.: 1970, Astrophys. J. 162, 1003.Google Scholar
Kane, S. R. and Donnelly, R. F.: 1971, Astrophys. J. 164, 151.Google Scholar
Kane, S. R. and Lin, R. P.: 1972, Solar Phys. 23, 457.Google Scholar
Krieger, A., Paolini, F., Vaiana, G. S., and Webb, D.: 1972, Solar Phys. 22, 150.Google Scholar
Lin, R. P.: 1970, Solar Phys. 12, 209.Google Scholar
Lin, R. P.: 1973, in Ramaty, R. and Stone, R. G. (eds.), High Energy Phenomena on the Sun, NASA SP-342, p. 439.Google Scholar
Lin, R. P. and Hudson, H. S.: 1971, Solar Phys. 17, 412.Google Scholar
Lin, R. P. and Anderson, K. A.: 1967, Solar Phys. 1, 446.Google Scholar
Lin, R. P., Evans, L. G., and Fainberg, J.: 1973, Astrophys. Letters 14, 191.Google Scholar
McDonald, F. B. and Van Hollenbecke, M.: 1973, in Ramaty, R. and Stone, R. G. (eds.), High Energy Phenomena on the Sun, NASA SP-342, p. 404.Google Scholar
McKenzie, D. L., Datlowe, D. W., and Peterson, L. E.: 1973, Solar Phys. 28, 175.Google Scholar
Peterson, L. D., Datlowe, D. W., and McKenzie, D. L.: 1973, in Ramaty, R. and Stone, R. G. (eds.), High Energy Phenomena on the Sun, NASA SP-342, p. 132.Google Scholar
Smith, H. J. and Smith, E. P.: 1963, Solar Flares, MacMillan Co., New York.Google Scholar
Sweet, P. A.: 1969, Ann. Rev. Astron. Astrophys. 7, 149.Google Scholar
Syrovatskii, S. I.: 1969, in de Jager, C. and Švestka, Z. (eds.), Solar Flares and Space Research, North-Holland Publ. Co., Amsterdam, p. 346.Google Scholar
Tanaka, K. and Nakagawa, Y.: 1973, Solar Phys. 33, 187.Google Scholar
Takakura, T.: 1972, Solar Phys. 26, 151.CrossRefGoogle Scholar
Thomas, R. J. and Neupert, W. M.: 1971, Bull. A.A.S. 3, 264.Google Scholar
Trubnikov, B. A.: 1965, Rev. Plasma Phys. 1, 105.Google Scholar
Van Allen, J. A. and Krimigis, S. M.: 1965, J. Geophys. Res. 70, 5737.Google Scholar
Vorpahl, J. and Zirin, H.: 1970, Solar Phys. 11, 285.Google Scholar
Wild, J. P., Smerd, S. F., and Weiss, A. A.: 1963, Ann. Rev. Astron. Astrophys. 1, 291.Google Scholar