Radio Jupiter Observed From High Northern Latitudes

Details Radio Jupiter Observed From High Northern Latitudes Radio Jupiter Observed From High Northern Latitudes

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agusmsh21b..04k&link_type=abstract

American Geophysical Union, Spring Meeting 2004, abstract #SH21B-04

Astronomy and Astrophysics

Astronomy

2756 Planetary Magnetospheres (5443, 5737, 6030), 2784 Solar Wind/Magnetosphere Interactions, 5757 Remote Sensing, 6954 Radio Astronomy

Scientific paper

Radio observations of Jupiter during the Voyager fly-bys in 1979 and the Ulysses fly-by in 1992 revealed that dramatic changes in morphology occurred in conjunction with seemingly small changes in observer's Jovicentric latitude. Indeed, at sub-observer latitudes outside the nominal equatorial band observable from Earth, several new Jovian radio components were observed. During the later half of 2003 and most of 2004, the Ulysses spacecraft is performing another fly-by of Jupiter, but at a much greater distance (0.8 to ~2.0 AU) than during the 1992 fly-by (6 Jovian radii). However, even at these distances, Jupiter is the dominant radio source, permitting synoptic intensity and (occasionally) polarization observations to be made by the Ulysses radio and plasma wave instrument. During this distant fly-by, the Jovicentric latitude excursion is very large, covering the range from about +75 degrees down to -15 degrees while closer than 2 AU to Jupiter. Here we describe low frequency (<1 MHz) observations made during the northern phase of this fly-by, covering latitudes from +75 degrees to almost the equator, including some intervals at the same latitude but dramatically different local times. Perhaps the most persistent emissions observed at high latitudes are the so-called QP (quasi-periodic) bursts, although their appearance is much more complex than during the first Ulysses fly-by in 1992. Also evident are some broad band features that may be triggered by co-rotating solar wind structures. Coronal mass ejections (CMEs) are another contributor to the variability of Jovian radio emissions and we will show examples of enhanced Jovian emissions correlated with impact of CMEs with the Jovian magnetosphere during the extremely active solar storms of Oct-Nov 2003.

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