The radio signatures of a slow coronal mass ejection - Electron acceleration at slow-mode shocks
- Maryland Univ., College Park (USA)
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. 46 refs.
- OSTI ID:
- 6966926
- Journal Information:
- Astrophysical Journal; (USA), Journal Name: Astrophysical Journal; (USA) Vol. 347; ISSN ASJOA; ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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Related Subjects
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ACCELERATION
ALFVEN WAVES
ATMOSPHERES
ELECTROMAGNETIC RADIATION
HYDROMAGNETIC WAVES
INSTABILITY
MAGNETIC FIELDS
MASS TRANSFER
RADIATIONS
RADIOWAVE RADIATION
SATELLITES
SHOCK WAVES
SKYLAB
SOLAR ACTIVITY
SOLAR CORONA
SOLAR RADIO BURSTS
STELLAR ATMOSPHERES
STELLAR CORONAE