Balasubramaniam, K. S., Cliver, E. W., Pevtsov, A., Temmer, M., Henry,
T. W., Hudson, H. S., Imada, S., Ling, A. G., Moore, R. L., Muhr, N.,
Neidig, D. F., Petrie, G. J. D., Veronig, A. M., Vrsnak, B, White, S.
"On the Origin of the Solar Moreton Wave of 2006 December 6,"
ApJ 723, 587 (2010).
The Moreton wave has always been one of the more fascinating aspects of a solar flare, and this paper describes a wonderful one. The cartoon - well, it is just avoids the big issue here: is a one-wave description adequate, or must one have two? If one, it would be the bow shock known to precede the CME ejecta; if two the other would be a simple wave propagating as an MHD fast-mode shock. If one-wavism triumphs (and the Archivist thinks the data are thus far ambiguous on this point), then the flanks of the bow wave would have to provide the energy for the Moreton wave, which (as this cartoon nicely shows) resides at the bottom of the corona (the chromosphere, to be more precise). It is only that topmost dash in the shock shown here that suggests two-wavism: if it did not curve over like that, it would be a better representation of a bow wave.
October 26, 2010
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