Direction finding study of Jovian hectometric and broadband kilometric radio emissions: Evidence for their auroral origin

Details Direction finding study of Jovian hectometric and broadband kilometric radio emissions: Evidence for their auroral origin Direction finding study of Jovian hectometric and broadband kilometric radio emissions: Evidence for their auroral origin

Nov 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994p%26ss...42..919l&link_type=abstract

Planetary and Space Science (ISSN 0032-0633), vol. 42, no. 11, p. 919-931

Physics

Plasma Physics

39

Auroras, Direction Finding, Jupiter (Planet), Planetary Magnetic Fields, Planetary Magnetospheres, Plasma Physics, Radio Astronomy, Error Analysis, Radio Antennas, Radio Receivers, Ulysses Mission, Voyager 1 Spacecraft, Voyager 2 Spacecraft

Scientific paper

Taking advantage if the direction finding capabilities of the Ulysses unified radio and plasma wave (URAP) experiment we derive the source locations and emission characteristics of the Jovian hectometric (HOM) and broadband kilometric (bKOM) emissions. Unlike previous studies we additionally determine the systematic error of the source direction due to the uncertainty of the antenna/receiver calibration parameters. To obtain maximum accuracy when doing direction finding, we use HOM and bKOM events observed close to the Ulysses encounter with Jupiter. It is found that both emissions have their sources at the auroral zones of Jupiter, at dipole L shells between 7 and 11 for HOM in the northern hemisphere, and between 9 and 15 for the bKOM radiation observed at high southern latitudes after the Ulysses Jupiter encounter. For the analyzed HOM events the source location is usually between 40 deg and 130 deg central meridian longitude (CML) and 2200 and 0600 local time (LT), but probably there exist emissions from other longitudes and local times too. In contrast, the bKOM is emitted from a wide range of longitudes and local times as well. There is some evidence that both the kilometric and hectometric emissions are composed of a dominant component in the fast extraordinary (R-X) mode and a weaker ordinary (L-O) mode component. Due to the uncertainty in source direction determination the emission's cone half-angle (i.e. half-angle of the cone in which the emission is beamed) cannot be accurately determined. It is some 30 deg - 90 deg for the HOM and about 40 deg - 80 deg for the bKOM. The source location of bKOM is likely to be associated with open magnetospheric field lines whereas the HOM radio sources with the inner Jovian plasma sheet and/or outer plasma torus. There is some evidence that the bKOM radio emissions are correlated with ultraviolet auroral activity.

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