Jupiter's most powerful radio emissions: vlf

Details Jupiter's most powerful radio emissions: vlf Jupiter's most powerful radio emissions: vlf

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja.....1920k&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #1920

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Scientific paper

At frequencies just above the solar wind plasma frequency, Jupiter emits perhaps its most powerful radio bursts, observable over distances of several AU. Originally called escaping continuum emission, this component may actually be the amalgamation of all of the Jovian low frequency bursts whose lowest frequency portions have their group velocities slowed to almost zero as they transit the Jovian magnetosheath, thus forming an amorphous quasi-continuous band dubbed reradiated emission. As observed by spacecraft sunward of Jupiter, the very lowest frequency portion of this band exhibits a sharp cutoff corresponding to the plasma frequency near the nose of the Jovian magnetosheath, just inside the magnetopause. Observations of the variations of the cutoff frequency provide a remote measure of the solar wind ram pressure at Jupiter. At times, the total integrated power in this oft-neglected portion of the Jovian radio spectrum may exceed that of all other radio sources, if one assumes it is radiated into all directions. In fact, new observations by the widely separated Cassini and Ulysses spacecraft and the Galileo spacecraft inside the Jovian magnetosphere reveal that the emission is of the strobe light variety, i.e. emitted in all directions simultaneously, as opposed to a search light type of emission which rotates with the planet. These new observations also reveal some intriguing differences in the observed spectrum, consistent with an extended magnetosheath source. The morphology of these reradiated emissions will be described and a possible model for their origin will be discussed.

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