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Дата последнего поиска статьи во внешних источниках: 18 июля 2013 г.
Аннотация:Differences in the solar wind interaction with the
magnetosphere of Saturn relative to the Earth result from the
decrease in the solar wind plasma density and magnetic field
strength with distance from the Sun, and from the change in
the average angle of the IMF at Saturn’s orbit. Other reasons
are related to Saturn’s rapid rotation and internal magnetospheric
plasma sources. Moreover, the IMF structure observed
by Cassini in 2003–2004 during the approach to Saturn
is consistent with corotating interaction regions (CIRs)
existing during the declining phase of the solar cycle. Two
cases on 16 and 26 January 2004 are considered when disturbances
in the solar wind passed Cassini and then Saturn.
After the solar wind shock encountered the kronian magnetosphere,
the auroral oval became brighter (especially at dawn)
with a reduced radius. In these cases the auroral power was
anti-correlated with the radius of the oval. Possible mechanisms
responsible for such unexpected behavior are presented
and discussed in detail.