Jupiter's Magnetosphere

Earth's magnetic field creates a 'bubble' around Earth that helps protect our planet from some of the more harmful effects of energetic particles streaming out from the sun in the solar wind. Some of the earliest hints of this interaction go back to the 1850s with the work of Richard Carrington, and in the early 1900s with the work of Kristian Birkeland and Carl Stormer. That this field might form a type of 'bubble' around Earth was hypothesized by Sidney Chapman and Vincent Ferraro in the 1930s. The term 'magnetosphere' was applied to magnetic bubble by Thomas Gold in 1959. But it wasn't until the Space Age, when we sent the first probes to other planets, that we found clear evidence of their magnetic fields (though there were hints of a magnetic field for Jupiter in the 1950s, due to observations from radio telescopes).

The Voyager program, two spacecraft launched in 1977, and successors to the Pioneer 10 and 11 missions, completed flybys of the giant outer planets. They became the implementation of the 'Grand Tour' of the outer planets originally proposed in the late 1960s. The Voyagers provided some of the first detailed measurments of the strength, extent and diversity of the magnetospheres of the outer planets.

In this series of visualizations, we present simplified models of these planetary magnetospheres, designed to illustrate their scale, and basic features of their structure and impacts of the magnetic axes offset from the planetary rotation axes.

The volcanic activity on Jupiter's moon Io launches a large amount of sulfur-based compounds along its orbit, which is subsequently ionized by solar ultraviolet radiation. This is represented in the visualization by the yellowish structure along the orbit of Io. This creates a plasma torus and ring current around Jupiter, which alters the planet's magnetic field, forming some of the perturbations in Jupiter's magnetic field along the orbit of Io.

For these visualizations, the magnetic field structure is represented by gold/copper lines. The semi-transparent grey mesh in the distance represents the boundary of the magnetosphere. Major satellites of the planetary system are also included. When appropriate for the time window of the visualization, the Voyager flyby trajectories are indicated.

The models are constructed by combining the fields of a simple magnetic dipole, a current sheet (whose intensity is tuned match the scale of the magnetotail), and occasionally a ring current. This is a variation of the simple Luhmann-Friesen magnetosphere model. They are meant to be representative of the basic characteristics of the planetary magnetic fields. Some features NOT included are longitudes of magnetic poles to a standard planetary coordinate system and offsets of the dipole center from the planetary center.

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References

• T. Gold, Motions in the Magnetosphere of the Earth
• Luhmann and Friesen, A simple model of the magnetosphere
• LASP: Polarity of planetary magnetic fields
• Wikipedia: The Solar Storm of 1859
• Wikipedia: Kristian Birkeland
• Wikipedia: Carl Størmer

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Special thanks to Arik Posner (NASA/HQ) and Gina DiBraccio (UMBC/GSFC) for helpful pointers on orientation of planetary rotation and magnetic axes.