Hostname: page-component-586b7cd67f-t8hqh Total loading time: 0 Render date: 2024-11-28T09:24:12.903Z Has data issue: false hasContentIssue false
  • English
  • Français

Energetic Solar Electrons – Whistler Bootstrap, Magnetic Knots and Small-scale Reconnection

Published online by Cambridge University Press:  08 June 2011

Ilan Roth
Ilan Roth*
Affiliation:
Space Sciences, University of California at Berkeley, Berkeley, CA 94720, USA email: [email protected]
Rights & Permissions [Opens in a new window]

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.

The (near) relativistic electrons, emanating from the solar corona in long-lasting, gradual events, are generally observed at 1 AU as delayed vs the less energetic, type-III beams. The observations are consistent with the delayed electrons being energized along the stretched post-CME coronal field lines, when the tail of an anisotropic seed population, which is injected in conjunction to the observed radioheliograph bursts, interacts with the self-excited whistler waves (bootstrap mechanism). These bursts indicate efficient processes where suprathermal seed electrons are injected as a result of magnetic reconnection at the marginally stable coronal configuration left behind the emerging CME. The dependence of the bootstrap mechanism on the electron injection raises the general question of the MHD description and its deviation over the small electron skin-depth scale. The similarity between MHD and knot theories allows one to characterize any turbulent magnetic configuration through topological invariants, while deviation over electron skin-depth scale, characterized by the generalized vorticity, which is enhanced due to density inhomogeneity, creates the conditions for the potential injection sites.

Keywords

relativistic electronssolar flaresknotsreconnection
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S274: Advances in Plasma Astrophysics , September 2010 , pp. 178 - 181
Copyright
Copyright © International Astronomical Union 2011

References

Alexander, J. W., Trans Amer Math Society, 30, 275, 1928.CrossRefGoogle Scholar
Hass, J. and Lagarias, J., J. Amer. Math. Soc. 14, no. 2, 399, 2001.CrossRefGoogle Scholar
Jones, V., Bull. Am. Math. Soc. 12, 103–111, 1985.CrossRefGoogle Scholar
Klassen, A. S. et al. ., Geoph. Res., 110, AO9S04, 2005.CrossRefGoogle Scholar
Krucker, S., et al. ., Astrophys. J., 519, 864, 1999.CrossRefGoogle Scholar
Maia, D. J. F. et al. ., Astrophys. J., 660, 874, 2007.CrossRefGoogle Scholar
Mozer, F. S. et al. ., Phys Rev Lett, 91, 245002, 2003.CrossRefGoogle Scholar
Mozer, F. S., Jour, Geoph, Res., 1190, A12222, 2005.Google Scholar
Reidemeister, K., Abh. Math. Sem. Univ. Hamburg 5 24–32, 1926.CrossRefGoogle Scholar
Roth, I., Jour Atmospheric Solar-Terrestrial Phys., 70, 490, 2008.CrossRefGoogle Scholar