The latter part of Section 1.4 describes Jupiter's enormously strong magnetic field, and Section 1.3 mentions the associated radiation belt of magnetically-confined charged particles that are liable to damage the electronics of any spacecraft that lingers too long. Figure 2 shows views of the inner and most intense part of the radiation zone. Another version is shown in Figure 3.
Figure 4 shows a greater extent of the radiation zone detected by a different method. A colour version of Figure 5 showing an aurora where the magnetic field channels charged particles into the atmosphere appears as Figure 6, and a more powerful and spectacular aurora recorded in the ultraviolet is shown in Figure 7.
The strong radiation zone in Figure 2 is actually hoop-like in shape, and runs right round the planet. However, the figure makes it look like separate patches to either side of the globe because this is where our line of sight passes through the greatest extent of the zone. To visualize this, imagine sticking a knitting needle into a ring doughnut: a needle pointing towards the centre would only pass through a couple of centimetres before reaching the hole, whereas a needle parallel to this but off to the side would miss the hole and pass through a lot more cake before emerging again.
Bearing in mind information given in Section 1.4, why do you think the location of the radiation belt relative to the planet appears to change between the two images in Figure 2?
The two images were obtained half a rotation apart, and the 'wobble' in the orientation of the radiation belt arises because the axis of the magnetic field is tilted relative to Jupiter's rotation axis (by nearly 10° according to Section 1.4.
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