The radio signatures of a slow coronal mass ejection - Electron acceleration at slow-mode shocks?

Details The radio signatures of a slow coronal mass ejection - Electron acceleration at slow-mode shocks? The radio signatures of a slow coronal mass ejection - Electron acceleration at slow-mode shocks?

Dec 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...347..505k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 347, Dec. 1, 1989, p. 505-513. Research supported by the University of Mary

Astronomy and Astrophysics

Astrophysics

13

Coronal Loops, Particle Acceleration, Radio Emission, Shock Waves, Solar Corona, Skylab Program, Solar Magnetic Field, Solar Maximum Mission, Type 2 Bursts, Type 4 Bursts

Scientific paper

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.

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