Hostname: page-component-cd9895bd7-gvvz8 Total loading time: 0 Render date: 2024-12-12T19:52:44.310Z Has data issue: false hasContentIssue false
  • English
  • Français

Acceleration Mechanisms, Flares, Magnetic Reconnection And Shock Waves

Published online by Cambridge University Press:  30 March 2016

Stirling A. Colgate
Stirling A. Colgate*
Affiliation:
University of California, Los Alamos Scientific Laboratory Los Alamos, NM 87544, USAandNew Mexico Institute of Mining and TechnologySocorro, NM 87801, USA

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.

Acceleration in astrophysics usually means converting a significant fraction of the energy of some source into particles whose individual kinetic energy greatly exceeds the average temperature of the medium. There are three general classifications of acceleration processes. The first is hydrodynamic, second coherent electromagnetic, and third stochastic electromagnetic processes. We shall discuss each of these briefly in terms of the spectrum of accelerated particles. This can be related to an efficiency by the relationships N(>E) α E┌ or an energy efficiency N(>E) α EI-г In astrophysics we frequently emphasize Г without realizing the constraints this imposes upon the efficiency of the acceleration mechanism. So often the relatively flat spectra result in efficiency requirements that challenge the ingenuity of those who wish to invent acceleration mechanisms.

Type
Joint Discussion
Information
Highlights of Astronomy , Volume 5: Highlights of Astronomy. As presented at the XVIIth General Assembly of the IAU, 1979 , 1980 , pp. 397 - 410
Copyright
Copyright © Cambridge University Press 1980

References

Benz, A.O. (1979) Ap. J. 211, 270.CrossRefGoogle Scholar
Blanford, R.D. and Ostriker, J.P. (1978) Ap. J. Lett. 221, 229.Google Scholar
Chin-Fatt, C. (1974) Phys. Fluids 17, 1410.Google Scholar
Colgate, S.A. (1975) Ap. J. 198, 439.CrossRefGoogle Scholar
Colgate, S.A., (1975) “Origin of Cosmic Rays,” Osborne, J. and Wolfendale, A.W. (eds.) pp. 447-466, Reidel Publ. Co., Holland.Google Scholar
Colgate, S.A. (1977) “Thermal X-Rays and Deuterium Production in Stellar Flares, 15th International Cosmic Ray Conference, Plovidv, Bulgaria, Sp. 3, p. 6.Google Scholar
Colgate, S.A., (1978) Ap. J. 221., 1068.CrossRefGoogle Scholar
Colgate, S.A. and Johnson, M.H., (1960) Phys. Rev. Lett. 5, 235.Google Scholar
Colgate, S. A, McKee, C.R., and Blevins, B., (1972) Ap. J. 173, L87.Google Scholar
Colgate, S.A. and Petschek, A.E., (1979) Ap. J. 229, 682.Google Scholar
Colgate, S.A. and White, R.H., (1966) Ap. J. 143, 626.Google Scholar
Dawson, J. and Oberman, C. (1963) Phys. Fluid 6, 390.Google Scholar
Drake, J.F. and Lee, Y.C. (1977) Phys. Rev. Lett 39, 453.Google Scholar
Fujimoto, Y. and Mishkin, E., (1978) Phys. Fluids 21, 1933.Google Scholar
Furth, H.P., Killeen, J., and Rosenbluth, M., (1963) Phys. of Fluids 6, 459.Google Scholar
Galeev, A.A. (1978) Phys. of Fluids, 21, 1353.Google Scholar
Grover, R. and Hardy, J., (1966) Ap. J. 143, 48.Google Scholar
Guderley, G., (1942) Luftfahrt Forschung, 19, 302.Google Scholar
Hamberger, S.M., Jancarik, J., Sharp, L.E., Aldcroft, D.A., and Wetherell, A. (1971) Plasma Physics and Controlled Nuclear Fusion Research, Vol. II, p. 37.Google Scholar
Hoyng, P. (1975) “Studies on Hard X-Ray Emission from Solar Flares on Radiation from the Cold on M Plasma,” (Ph.D. thesis UHTREX).Google Scholar
Hoyng, P. (1977) Astron. Astrophys. 55, 31.Google Scholar
Johnson, M.H. and McKee, C.F. (1971) Phys. Rev. D. 3, 4858.Google Scholar
Blanford, R.D. (1979) “Fermi Acceleration by Shocks,” ed. J., Arons, Workshop on Particle Acceleration Mechanisms in Astrophysics, LaJolla Institute, LaJolla, CA. Google Scholar
Krall, N.A. (1974) ed. Jr.Newkirk, G., Coronal Disturbances (Proceedings IAU Symposium 57, Surfers Paradise 1973), p. 365.CrossRefGoogle Scholar
Krall, N.A. (1979) “Fermi Acceleration by Shocks,” ed. J., Arons, Workshop on Particle Acceleration Mechanisms in Astrophysics, LaJolla Institute, LaJolla, CA.Google Scholar
Kulsrud, R.M., Ostriker, J.P., and Gunn, J.E. (1972) Phys. Rev. Lett. 28, 636.Google Scholar
McKee, C.R. and Colgate, S.A. (1973) Ap. J. 181, 903.CrossRefGoogle Scholar
McMillan, E.M. (1950) Phys. Rev. 79, 498.Google Scholar
Mullan, D.J., (1976) Ap. J. 208 199.Google Scholar
Noerdlinger, P.D. (1971) Phys. Fluids, 14, 999.CrossRefGoogle Scholar
Ono, Y., Skashita, S., and Ohyama, N. (1961) Progr. Theoret. Phys. Suppl. 20, 85.CrossRefGoogle Scholar
Parker, E.N., 1966, Ap. J. 145, 811.CrossRefGoogle Scholar
Petschek, H., (1964) in Hess, W.N. (ed.) “The Physics of Solar Flares,” NASA SP-50, p. 425.Google Scholar
Pikel’ner, S.B., Tsyovich, V.W. (1975) Astron. Zh. 52, 378 [Soviet Astron. Aj. 19, 450 (1976)].Google Scholar
Tsytovich, V. N, Stenflo, L. and Wilhelmsson, H. (1975) Physica Scripta 11, 251.Google Scholar
Vlakos, L. and Papadopoulos, K. (1979) “On the Impossibility of Up Conversion of Ion Sound the Langmuir Turbulence,” preprint, University of Maryland, College Park, MD.Google Scholar
White, R.B., Monticello, D., Rosenbluth, M.N., and Waddell, B.V. (1977) Phys. of Fluids 20, 800.Google Scholar
Yeh, Y. (1976), J. G. R. 81, 4524.Google Scholar