Modeling the Jovian Magnetospheric System II: Ionospheric Outflow

About this series of simulations:

A 3-D Multi-fluid simulation was used to examine both large and small scale features in the Jovian magnetospheric system.  It has been demonstrated by several reserachers (cf. Ogino et al., 1998, and Walker et al., 2001) that while variability in the incident solar wind plays a role in shaping the Jovian magnetosphere, the inner magnetsophere (<50Jupiter radii) is for the most part uneffected.  Unlike the Earth's magnetsophere where signifigant changes can be observed and modelled for solar wind variations on realistic timescales, the shear size of the Jovian magnetosphere would require long periods of contiuous solar wind for modifications to essentially convect into the inner magnetosphere. Therefore it is important to study the effects of the ionosphere a  plasma source governing inner magnetospheric dynamics.  The following parameter study included an examination of the global effects of different ionospheric outflow rates.  As stated on the previous page (initial case study), 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.  Images can be enlarged by clicking on them.     

	Side view of the magnetic field lines around Jupiter, including a density slab in the ecliptic plane.  This was for a high ionospheric outflow of 4*1030 amu/s determined at 2 Jupiter radii (RJ).
	A similar representation of the Jupiter system for a simulation with an outflow of 1030amu/s.  Notice the location of the bow shock (here it lies at about 90 RJ as opposed to 120 and expanding for the high outflow case).
	A top down view of the solar wind density for the high outflow case.  Both the distance of the bow shock and the extent to which the solar wind is held out of the magnetsophere are evident.
	A similar representation of the low outflow scenario.
	The silver sphere is 2RJ and the density slab is of O+.  The Io plasma torus is clearly resolved at 6RJ, and though some density diffusion occurs, it is for the most part a static feauture.
	The multi-fluid treatment allows for differential heating between plasma species.  Here the two slabs are of O+ temperature, demostrating regions of intense heating and energization.  (Sorry about the simulation units, I'll fix it soon!)
	Just a fun rendering of what I have in mind for my thesis project... complete integration of Ganymede and Jupiter simulations allowing  dynamic feedback between global and local simulations.

Who's Doing It:

• Robert M. Winglee.
• Carol Paty.
• Erika Harnett .