by ISEE 3/ICE, Geophys. Res. Lett., 17, 753, 1990.
Figure 1: Velocity distribution functions in the V
-V
plane for a rapid crossing of the current sheet during the Galileo
Earth1 flyby. Here V
and V
are the components
of the particle velocities along the designated GSE axes. The flow
is directed earthward. [Figure 6 of Frank et al., 1994b].
Figure 2: A simplified schematic diagram showing the diverse
trajectories of particles that form the distributions observed
during the Galileo Earth1 flyby. Here the (magnetic) neutral line
is defined as the locus across which the z-component of the
magnetic field, B
, reverses sign. An electric field, E,
is imposed in the y-GSE direction. The role of nonadiabatic
acceleration in the magnetotail current sheet is evident. [Figure
12 of Frank et al., 1994b].
Figure 3: Sketch of the inflowing (cold) and outflowing (heated) ion
distribution functions based on an analysis of individual particle
behavior in a curved magnetotail geometry. As above, the unprimed
velocity-space axes, V
-V
, can be taken as components
in GSE. The primed velocity-space axes represent particle
velocities measured in the rest frame of the convecting plasma.
This representation shows what happens if energy is conserved in
the non-convecting frame but pitch angle scattering is allowed to
occur. [Figure 1b of Cowley, 1984].
Figure 4: From top to bottom, the total plasma pressure ( P
=the sum of ion plus electron pressures= P
P
), magnetic
pressure ( B
/2
), total (plasma plus magnetic)
pressure, and plasma 
(ratio of plasma pressure to magnetic
pressure). All pressures are given in Pa. [Figure 4 of Frank
et al., 1994b].
Figure 5: The inbound trajectory of Galileo for the Earth2 flyby.
The trajectory is shown as 
vs. x where 
= (
y
+ z
)
, and an aberrated GSE coordinate system is
used. Galileo approached the Earth from the southern dusk
hemisphere. Locations of bow shock crossings are indicated with +
and o for inbound and outbound crossings, respectively. Fits to
the locus of the shock surface are also shown. The surface is in
all cases assumed to be hyperbolic in cross-section and the fits
are of the form 
. The Fairfield
[1971] curve adopted by Greenstadt
Figure 5 continued:
et al. [1990] has A,
B, C = 0.04, 45.3, 645, with no dependence on the IMF. For the
Galileo fits [A. Prevost et al., personal communication, 1994],
the coefficients depend on the orientation of the IMF and have the
values A, B, C = 0.14, 46.8, 730 for the perpendicular limit
and are close to the Greenstadt et al. fit for the parallel
limit.
Figure 6: The three GSE components of the magnetic field and the
field magnitude from the Galileo magnetometer [ Kivelson et
al., 1992] for six hours on December 5, 1992 during which the
trajectory skimmed the Earth's bow shock at a downtail distance
near 300 R
. Three pairs of shock crossings are shown.
Intervals in the magnetosheath are shaded. The shocks themselves
are in each case quasi-perpendicular. The field magnitude
increases by 
35% each time the spacecraft crosses into the
magnetosheath. The final inbound shock crossing was unclear in the
magnetometer data because the solar wind was highly disturbed.
Figure 7: Four second averages of the magnetic field vectors
projected into the xy plane (see text for definition of the
coordinates) and plotted along the projected trajectory of Galileo.
The base of each vector is set on the trajectory. Gaspra is not to
scale. A schematic magnetosphere and whistler fronts that bound
the region of disturbance are also shown. [Figure 3 of
Kivelson et al., 1993b].