Physics of Plasmas
Feedback | Help | Exit
Physics of Plasmas
Search:
   
 
 
 
Previous Article
Study of fast-electron transport in laser-illuminated spherical targets
The transport and scattering of fast electrons created by the two-plasmon-decay instability are studied by comparing the hard x-ray signal from two identically irradiated targets: a 1-mm-diam solid Cu...
Next Article
Kinetic theory for the ion humps at the foot of the Earth's bow shock
The nonlinear kinetic theory is presented for the ion acoustic perturbations at the foot of the Earth's quasiperpendicular bow shock, that is characterized by weakly magnetized electrons and unmagneti...

Nonlinear evolution of Buneman instability and its implication for electron acceleration in high Mach number collisionless perpendicular shocks

Phys. Plasmas 16, 102901 (2009); doi:10.1063/1.3240336

Published 1 October 2009

You are logged in to this journal.

Takanobu Amano1 and Masahiro Hoshino2
1Department of Physics, Nagoya University, Nagoya 464-8602, Japan
2Department of Earth and Planetary Science, University of Tokyo, Tokyo 113-0033, Japan
Nonlinear evolution of the Buneman instability and its application to electron acceleration in collisionless shocks are discussed. Two-dimensional particle-in-cell simulations show that the saturation level of the instability is reduced from one-dimensional simulation results. It is demonstrated that the reduced saturation level is due to the resonant wave-particle interactions with large amplitude obliquely propagating waves. A new estimate for the saturation level is given by considering the interactions with oblique modes. The effects of the large amplitude oblique modes on electron shock surfing acceleration that is mainly controlled by the Buneman instability are also investigated. Two-dimensional particle-in-cell simulations of the shock transition region are performed by adopting a local model with the periodic boundary condition. The results indicate that the presence of oblique modes introduces a stochastic behavior to the trajectories of energetic electrons. The maximum energy is limited by the finite lifetime of the instability in the present periodic model. However, this will not be the case in the realistic shock transition region. The application to realistic shocks with Mach numbers typical of supernova remnants is also discussed. ©2009 American Institute of Physics
History: Received 22 June 2009; accepted 8 September 2009; published 1 October 2009
Permalink: http://link.aip.org/link/?PHPAEN/16/102901/1
FULL TEXT OPTIONS   (FREE)
Download PDF (1663 kB) View Cart

KEYWORDS and PACS

Keywords
PACS
  • 52.35.Py
    Plasma macroinstabilities (hydromagnetic)
  • 52.35.Tc
    Shock waves and discontinuities in plasma
  • 52.65.Rr
    Particle-in-cell method (plasma simulation)
  • 94.30.cq
    MHD waves, plasma waves, and instabilities in the magnetosphere
  • 52.35.Mw
    Nonlinear phenomena: plasma waves, wave propagation and other interactions
  • YEAR: 2009

RELATED DATABASES

Web of Science

View this record in Web of Science

PUBLICATION DATA

ISSN:
1070-664X (print)   1089-7674 (online)
Publisher:
AIP is a member of CrossRef AIP

REFERENCES (29)
View in Separate Window/Tab
  1. H. Matsumoto, H. Kojima, T. Miyatake, Y. Omura, M. Okada, I. Nagano, and M. Tsutsui, Geophys. Res. Lett. 21, 2915, doi:10.1029/94GL01284 (1994).
  2. I. B. Bernstein, J. M. Greene, and M. D. Kruskal, Phys. Rev. 108, 546 (1957).
  3. Y. Omura, H. Kojima, and H. Matsumoto, Geophys. Res. Lett. 21, 2923, doi:10.1029/94GL01605 (1994). [ISI]
  4. R. E. Ergun, C. W. Carlson, J. P. McFadden, F. S. Mozer, G. T. Delory, W. Peria, C. C. Chaston, M. Temerin, I. Roth, L. Muschietti, R. Elphic, R. Strangeway, R. Pfaff, C. A. Cattell, D. Klumpar, E. Shelley, W. Peterson, E. Moebius, and L. Kistler, Geophys. Res. Lett. 25, 2041, doi:10.1029/98GL00636 (1998). [ISI]
  5. C. Cattell, J. Crumley, J. Dombeck, J. Wygant, and F. S. Mozer, Geophys. Res. Lett. 29, 1065, doi:10.1029/2001GL014046 (2002).
  6. S. D. Bale, P. J. Kellogg, D. E. Larson, R. P. Lin, K. Goetz, and R. P. Lepping, Geophys. Res. Lett. 25, 2929, doi:10.1029/98GL02111 (1998).
  7. O. Buneman, Phys. Rev. Lett. 1, 8 (1958).
  8. J. F. Drake, M. Swisdak, C. Cattell, M. A. Shay, B. N. Rogers, and A. Zeiler, Science 299, 873 (2003). [MEDLINE]
  9. K. Papadopoulos, Astrophys. Space Sci. 144, 535 (1988). [Inspec] [ISI]
  10. T. Amano and M. Hoshino, Astrophys. J. 661, 190 (2007).
  11. M. Hoshino and N. Shimada, Astrophys. J. 572, 880 (2002).
  12. O. Ishihara, A. Hirose, and A. B. Langdon, Phys. Fluids 24, 452 (1981).
  13. R. C. Davidson, N. A. Krall, K. Papadopoulos, and R. Shanny, Phys. Rev. Lett. 24, 579 (1970). [ISI]
  14. M. E. Dieckmann, P. Ljung, A. Ynnerman, and K. G. McClements, Phys. Plasmas 7, 5171 (2000). [ISI]
  15. M. Lampe, I. Haber, J. H. Orens, and J. P. Boris, Phys. Fluids 17, 428 (1974).
  16. R. L. Morse and C. W. Nielson, Phys. Rev. Lett. 23, 1087 (1969).
  17. D. Biskamp and R. Chodura, Phys. Rev. Lett. 27, 1553 (1971).
  18. C. T. Dum and K. -I. Nishikawa, Phys. Plasmas 1, 1821 (1994). [ISI]
  19. N. Shimada and M. Hoshino, Astrophys. J. Lett. 543, L67 (2000).
  20. T. Katsouleas and J. M. Dawson, Phys. Rev. Lett. 51, 392 (1983).
  21. R. Blandford and D. Eichler, Phys. Rep. 154, 1 (1987). [Inspec] [ISI]
  22. Y. Ohira and F. Takahara, Astrophys. J. Lett. 661, L171 (2007).
  23. T. Amano and M. Hoshino, Astrophys. J. 690, 244 (2009).
  24. S. Matsukiyo and M. Scholer, J. Geophys. Res. 108, 1459, doi:10.1029/2003JA010080 (2003).
  25. S. Matsukiyo and M. Scholer, J. Geophys. Res. 111, A06104, doi:10.1029/2005JA011409 (2006).
  26. M. E. Dieckmann, A. Bret, and P. K. Shukla, New J. Phys. 10, 013029 (2008).
  27. M. E. Dieckmann, K. G. McClements, S. C. Chapman, R. O. Dendy, and L. O. C. Drury, Astron. Astrophys. 356, 377 (2000). [Inspec] [ISI]
  28. K. G. McClements, M. E. Dieckmann, A. Ynnerman, S. C. Chapman, and R. O. Dendy, Phys. Rev. Lett. 87, 255002 (2001). [ISI] [MEDLINE]
  29. N. Shimada, T. Terasawa, M. Hoshino, T. Naito, H. Matsui, T. Koi, and K. Maezawa, Astrophys. Space Sci. 264, 481 (1998). [Inspec]






Copyright © American Institute of Physics