Recurring Episodes of Jovian Radio Emission Driven by Magnetospheric Interaction with Corotating Solar Wind Density Structures and Sector Boundaries

Details Recurring Episodes of Jovian Radio Emission Driven by Magnetospheric Interaction with Corotating Solar Wind Density Structures and Sector Boundaries Recurring Episodes of Jovian Radio Emission Driven by Magnetospheric Interaction with Corotating Solar Wind Density Structures and Sector Boundaries

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agusmsh23a..02m&link_type=abstract

American Geophysical Union, Spring Meeting 2004, abstract #SH23A-02

Astronomy and Astrophysics

Astronomy

2756 Planetary Magnetospheres (5443, 5737, 6030), 5737 Magnetospheres (2756), 6220 Jupiter, 6954 Radio Astronomy

Scientific paper

In 2003 and early 2004, the Ulysses spacecraft descended from high heliographic latitudes towards perihelion, bringing it relatively close to Jupiter. The geometry of this distant flyby (0.8 AU closest approach) caused Ulysses to spend more than 6 months above a jovicentric latitude of 50 deg at a range of less than 2 AU, while the spacecraft traversed a considerable range of Jovian local time (9 hrs to 17 hrs). During much of this time interval, Jupiter was intercepted each solar rotation by two corotating high density structures and sector boundaries. From the perspective of Ulysses, the radio response of the magnetosphere to a given corotating structure was the intensification of either Jovian broad-band kilometric (bKOM) emission or of a combination of emissions, including bKOM and Jovian narrow-band kilometric (nKOM) emission. Such enhancements have been studied previously with Voyager, Ulysses, Galileo, and Cassini radio data. For Ulysses observations in 1991 and 1992, in particular, the typical scenario was brightening in the Jovian bKOM emission, followed by a sudden cessation of the bKOM emission and an onset of an nKOM "event" that lasted for some 120 hours (Reiner et al., 2000). For the sequences of events in 2003-2004, the two episodes per solar rotation clearly have different morphologies. These differences provide a unique opportunity to study solar wind and interplanetary magnetic field interaction with the Jovian magnetosphere over a period of 6 months, with upstream data provided by the Ulysses solar wind and magnetic field instruments. The goal is to determine which inputs to the magnetosphere are the most influential, resulting in different magnetospheric and, consequently, radio emission responses.

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