Abstract
Spectrographic and imaging observations of meter wave fast drift bursts are presented which imply the quasi-simultaneous particle acceleration at two different sites in the corona: one below 0.5 R ⊙, where electron beams rising in the corona are produced, and one above 1.0 R ⊙ from which electron beams propagate downward as revealed by reverse drift bursts. This configuration produces three groups of bursts with a similar spatial brightness distribution during 2.5 hours, demonstrating the overall stability of the large-scale magnetic field structure. The source structure of the reverse drift bursts is consistent with particle acceleration in a coronal helmet streamer neutral sheet. The same kind of high coronal acceleration sites is necessary for explaining the energy spectrum observed in interplanetary electron events.
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