A New Solar Radio Emission Component Observed at Hectometric Wavelengths

Details A New Solar Radio Emission Component Observed at Hectometric Wavelengths A New Solar Radio Emission Component Observed at Hectometric Wavelengths

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja.....4451r&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #4451

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Scientific paper

From May 17 to 22, 2002 a highly circularly polarized solar radio source was observed by the WAVES receivers on the Wind spacecraft. This unique event, which became quite intense and definite after May 19 and which was observed continuously for 6 days, was characterized by fine frequency structures, 1 to 2 hour amplitude periodicities, and a peaked frequency spectrum. Indeed, this emission has characteristics more typical of planetary emissions than of solar emissions. This is the only such event observed by Wind/WAVES in its 8 years of operation. (The only other example of an event of similar nature may have been observed more than 20 years ago by the ISEE-3 spacecraft.) The direction-finding analysis for this event indicates a relatively small radio source that may lie somewhere between 0.06 and 0.36 AU from the sun. The radiation from this event was very weak at the onset, being nearly an order of magnitude below the galactic background radiation level. It is speculated that this radio event may be a unique hectometric manifestation of a moving type IV burst. The radiation mechanism is unknown--possibilities include plasma emission, gyro-synchrotron, and cyclotron maser.

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