Hostname: page-component-586b7cd67f-rdxmf Total loading time: 0 Render date: 2024-11-23T20:56:12.215Z Has data issue: false hasContentIssue false
  • English
  • Français

Diffusive Shock Acceleration by Multiple Shocks

Published online by Cambridge University Press:  25 April 2016

D.B. Melrose  and
M.H. Pope
D.B. Melrose
Affiliation:
Research Centre for Theoretical Astrophysics, and Sir Frank Packer Department of Theoretical Physics, School of Physics, University of Sydney, NSW 2006
M.H. Pope
Affiliation:
Research Centre for Theoretical Astrophysics, and Sir Frank Packer Department of Theoretical Physics, School of Physics, University of Sydney, NSW 2006
Get access Rights & Permissions [Opens in a new window]

Abstract

Diffusive shock acceleration produces a power law momentum distribution f(p)α p−b, with b ≥ 4 for a single shock, and b = 4 for a single strong shock. It has been shown that the distribution for acceleration at a sequence of identical shocks is flatter, approaching f(p)α p−3 below a high energy knee, for an arbitrarily large number of shocks. We show how this flatter distribution arises and discuss the range of momenta over which it extends after a finite number of shocks.

Type
High Energy Astrophysics
Information
Publications of the Astronomical Society of Australia , Volume 10 , Issue 3 , 1993 , pp. 222 - 224
Copyright
Copyright © Astronomical Society of Australia 1993

Access options

Get access to the full version of this content by using one of the access options below. (Log in options will check for institutional or personal access. Content may require purchase if you do not have access.)

References

Achterberg, A., 1990, in Brinkman, W., Fabian, A.C. and Giovanelli, F. (eds), Physical Processes in Hot Cosmic Plasmas, Kluwer Academic Publishers, Dordrecht, p. 67.CrossRefGoogle Scholar
Axford, W.I., 1980, in Setti, G., Spada, G. and Wolfendale, A.W. (eds), Origin of Cosmic Rays, Reidel, Dordrecht, p. 339.Google Scholar
Axford, W.I., Leer, E. and Skadron, G., 1977, Proc. 15th Int. Cosmic Ray Conf., 11, 132.Google Scholar
Bell, A.R., 1978a and b, Mon. Not. R. astr. Soc., 182, 147 and 443.CrossRefGoogle Scholar
Blandford, R.D. and Eichler, D., 1987, Pyhys. Rep. 154, 1.CrossRefGoogle Scholar
Blandford, R.D. and Ostriker, F.R., 1978, Astrophys. J., 221, L29.CrossRefGoogle Scholar
Blandford, R.D. and Ostriker, J.P., 1980, Astrophys. J., 237, 793.CrossRefGoogle Scholar
Bogdan, T.J. and Volk, H.J., 1983, Astron. Astrophys., 122, 129.Google Scholar
Drury, L.O., 1983, Rep. Prog. Phys., 46, 973.CrossRefGoogle Scholar
Krimsky, G.F., 1977, (in Russian), Dokl. Akad. Nauk, SSSR 234, 1306.Google Scholar
Melrose, D.B., 1986, Instabilities in Space and Laboratory Plasmas, CUP.CrossRefGoogle Scholar
Moraal, H. and Axford, W.I., 1983, Astron. Astrophys., 125, 204.Google Scholar
Scholer, M., 1985, in Tsurutani, B.T. and Stone, R.G. (eds), Collisionless Shocks in the Heliosphere: Reviews of Current Research, American Geophysical Union, Washington DC, p. 287.CrossRefGoogle Scholar
Toptyghin, I.N., 1980, Space Sci. Rev., 26, 157.CrossRefGoogle Scholar
White, R.L., 1985, Astrophys. J., 289, 698.CrossRefGoogle Scholar