A plot of the magnetic field and solar wind parameters
from Oct. 18 through Oct. 20 is shown in Figure 1.
From top to bottom the figure shows the magnetic field
strength (B), the elevation (
)
and azimuth (
)
of the magnetic field direction, the proton
density (N), the most probable proton thermal speed
assuming an isotropic Maxwellian velocity distribution
(VT =
(2kT/m)),
and the magnitude of the bulk velocity (V). The magnetic
cloud is the region in which the direction of the strong
magnetic field rotated smoothly from south to north.
The speed of the cloud was
400 km/s, and one does not see the decrease in
speed from the front to the rear that is typical of
magnetic clouds at 1 AU. This speed profile indicates
that the cloud was "old" [Farrugia et al.,
1992; Oscherovich et al., 1993, 1995] and no longer
rapidly expanding; further studies of this observation
are needed. A shock wave was observed ahead of the
magnetic cloud on calendar day 291.445 (Oct. 18 at
hour 10.7,
1040
UT), probably produced by the supermagnetoacoustic
motion of the magnetic cloud relative to the solar
wind closer to the sun.
The magnetic cloud was being overtaken by a corotating
stream. A corotating shock driven by the stream entered
the rear of the magnetic cloud and was observed by
WIND at 292.744. The stream compressed the plasma and
field at the rear of the magnetic cloud. A stream interface
was seen at 292.954, characterized by an abrupt decrease
in density, a similar increase in temperature and a
peak in the magnetic field intensity. A corotating
stream, indicated by the low density and high temperature,
followed the stream interface. WIND was clearly in
the stream after
293.3, when the speed and temperature were high,
the density was low, and the magnetic field strength
was average. The region between the first stream interface
at 292.954 and 293.3 was complicated, owing to a second
density peak and several large changes in magnetic
field direction in that interval. This too is a subject
that merits further study.
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