Group planetary
magnetospheres -
Structure and dynamics depend on
Consequences of external plasma properties
The magnetic field orientation of external plasma also matters
Mirror mode waves in
Earth’s magnetosheath
Rotational forces produce a disk of current in Jupiter’s magnetosphere
Convection (or circulation)–
a form of interchange but there are differences
Like convection, interchange implies plasma transport
Form of interchange
at Jupiter
Interchange near Io
and
probably throughout magnetosphere
Galileo fields and particle instruments have identified a bursty pattern in various ways
C21 inbound: “plasmoid” near 26 RJ post midnight. Note negative Bq and Br, Bf perturbations.
Dynamic events
at Jupiter vs.
Earth’s substorms
Tail convective flows: bipolar signatures post midnight as suggested by Vasyliunas, ‘83
Jupiter’s coupled
atmosphere,
ionosphere,
magnetosphere system
Jovian UV aurora
J. Clarke,
U. Michigan
Auroras differ at Earth & Jupiter
What produces the local time structure of Jupiter’s aurora?
Does the solar wind control
dynamics
at Jupiter?
Contrary to intuition
we propose
Ganymede’s magnetosphere:
the other extreme
Topology familiar
(as illustrated by a vacuum field model)
but configuration is not
Convection in Ganymede’s magnetosphere
Closed field region supports “field line resonances”
Field line resonances probe ionospheric conductivity & plasma density
Why is the density low on “upstream” closed field lines?