Abstract
The 1998 January 21 halo coronal mass ejection was launched from high
southern latitudes in
association with a filament disappearance observed by
the Nobeyama
Radioheliograph.
Signatures of the initial destabilization of the filament were observed
by the Extreme-ultraviolaet
Imaging Telescope (EIT) on board the SOHO spacecraft and by the Soft
X-ray Telescope (SXT)
on board Yohkoh. The Wind/WAVES experiment observed a type II burst in
the 600-300 kHz
range. The data coverage for this event is unusually high and we make
use of it to understand the
origin and evolution of the eruption. We address several issues based on
these data: (i) relation
between filament eruption and arcade formation beneath the filament,
(ii) comparison between the
hot arcade formation in X-rays and EUV, (iii) relation between the
filament eruption and the
white light CME, (iv) relation between the CME and the interplanetary
shock inferred from the
WAVES data. A summary of near-surface activities associated with the
eruption can be seen in
the Figure 1.
Figure 1. SOHO/MDI longitudinal magnetogram, with radio filament (white
contours) and X-ray
emission (enclosed by dark lines) are overlaid. The thick white line
from E to W is the neutral line
over which the eruption took place. North is to the top and east is to
the left. F is the location
where the filament split at the time of eruption.