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The radio signatures of a slow coronal mass ejection - Electron acceleration at slow-mode shocks?The evolution of a coronal mass ejection (CME) event observed on February 17, 1985 is studied using two-dimensional radio imaging observations along with simultaneously obtained coronagraph observations. This event shows that a slow CME can be associated with type II and type IV radio bursts. The implications of the spatial association of the radio bursts with the CME are discussed. It is argued that the CME is due to an instability of the large-scale magnetic field in a helmet streamer and that the radio bursts are some of the responses to this instability. The new feature of this event is the clear association of the moving type IV burst with a CME traveling slower than the coronal Alfven speed. The structure of slow shocks driven by such a CME is discussed, and it is shown that shock drift and diffusive acceleration are ineffective. An acceleration mechanism involving current-driven lower hybrid waves is proposed.
Document ID
19900030595
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Kundu, M.
(Maryland Univ. College Park, MD, United States)
Gopalswamy, N.
(Maryland Univ. College Park, MD, United States)
White, S.
(Maryland Univ. College Park, MD, United States)
Cargill, P.
(Maryland Univ. College Park, MD, United States)
Schmahl, E. J.
(Maryland, University College Park, United States)
Date Acquired
August 14, 2013
Publication Date
December 1, 1989
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 347
ISSN: 0004-637X
Subject Category
Solar Physics
Accession Number
90A17650
Funding Number(s)
CONTRACT_GRANT: NAG5-950
CONTRACT_GRANT: NAGW-81
CONTRACT_GRANT: NSF ATM-88-16008
Distribution Limits
Public
Copyright
Other

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