Statistical studies of non-Io Jupiter DAM emissions observed at Nançay during solar cycle 23 (1995-2001)

Details Statistical studies of non-Io Jupiter DAM emissions observed at Nançay during solar cycle 23 (1995-2001) Statistical studies of non-Io Jupiter DAM emissions observed at Nançay during solar cycle 23 (1995-2001)

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsm41b1669e&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SM41B-1669

Astronomy and Astrophysics

Astronomy

2407 Auroral Ionosphere (2704), 2799 General Or Miscellaneous, 5443 Magnetospheres (2756), 6220 Jupiter, 6954 Radio Astronomy

Scientific paper

Non-Io (or Io-independent) Jupiter decameter emissions observed by the Nançay decametric array during the rising phase of solar cycle 23 (1995-2001) are studied. About 700 emissions have been recorded during that period. From the statistical studies, several conclusions were obtained. It was observed that most of emissions (~91%) are Right-Hand elliptically polarized and from the so-called "A" source (i.e. northern hemisphere and for Jovian longitude of observer in the range ~200° to 320°). The relative contributions to emissions is (in decreasing order) from sources "A", "B" (northern, 100°-200°), C (southern, 300°-400°), and D (southern, 0°-80°). Considering all emissions, the average duration is ~22 min, the average maximum frequency is ~24 MHz and the average power is ~2.4 dB above the sky background. RH emissions reach higher frequencies than LH (Left-Hand) ones. Their duration and average power are similar, but peak values are higher for RH emissions. The number of emissions roughly follows the sunspot cycle. In relation to the solar cycle variation, it was observed that Jupiter radio emissions have on the average a longer duration during the rising phase. The maximum frequency of emissions is similar on the average for all phases, but extreme values (maximum) are seen during rising and solar maximum epochs. The emissions power is higher during the rising and maximum phases (similar in both) than during solar minimum.

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