Modeling the Jovian Magnetospheric System
About the Models:
A 3-D Multi-fluid simulation was used to examine both large and small
scale features in the Jovian magnetospheric system. A nested grid system
was used to get the finest resolution and least amount of numerical diffusion
near Jupiter and Io. Multi-fluid simulations have a plethora of benefits,
especially with respect to a complicated system like Jupiter's where there
are several high mass ion species dominating the energy and momentum transport
of the inner and most likely outer magnetosphere. This phenomenon is
due to the rapid rotation of Jupiter and its magnetosphere, which preferentially
accelerates more massive ion species. It allows one to examine the
differential acceleration and heating between the heavy and light ion species,
and follow their flow trajectories. Below are a few examples
of what can be examined with the multi-fluid simulation.
|
Side view of the magnetic field
lines around Jupiter with highlighted flux tubes representative of those mapping to the Galilean satellites. |
|
A figure looking at the pole of
Jupiter, showing the bulk fluid flow with co-rotation and the Parker spiral. |
|
A 3-D density and flow plot for O
+ complete with resolved Io plasma torus, corotion out to ~16RJ and a distinct shear between inner and outer torus flows at about 5RJ. |
|
A 3-D density and flow plot for
H+. Note similar coration features to the O+ and a similar polar jet. |
|
A 3-D density and flow plot for the solar wind, note that the cusp flow does not actually reach Jupiter, but is turned around well above the planet. |
|
A 2-D density contour for O
+ with Io (Io not to scale), demonstrating the initialized torus did not drift after running the simulation. |
|
A 2-D density contour for H
+ shows centrifugal forces at work due to Jupiter's rapid rotation and corotation of its magnetosphere out to ~16RJ. |
Who's Doing It:
Modeling the Jovian Magnetospheric System / 28 Aug 2002 / winglee@geophys.washington.edu