Type U burst and CME in the solar wind

Details Type U burst and CME in the solar wind Type U burst and CME in the solar wind

Apr 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999georl..26.1089l&link_type=abstract

Geophysical Research Letters, Volume 26, Issue 8, p. 1089-1092

Astronomy and Astrophysics

Astrophysics

4

Solar Physics, Astrophysics, And Astronomy: Radio Emissions, Radio Science: Radio Astronomy, And Astronomy: Magnetic Fields

Scientific paper

A type U burst was observed on 22 June 1998 with the WAVES radio receivers on the Wind spacecraft. It descended in frequency from 5 MHz to the turning frequency of about 1 MHz. It is extremely rare that a U burst is observed at such a low frequency, well out in the solar wind. Using a density model to convert frequency to radial distance we find that the radio emission started at 3 Ro, and that the electron stream turned back toward the Sun at about 8 Ro. The probable origin of the energetic electrons was in a B 6.8 X-ray flare that was coincident with the onset time of the U burst. A series of images by the LASCO coronagraph show a slow (214 km/s) CME in progress on the west limb whose front was at 9 Ro at the time of the U burst. As no stable magnetic loops exist at radial distances such as 8-9 Ro, we attribute the U burst to a stream of energetic electrons accelerated in an active region at the footpoint of one leg of the expanding arch of the CME.

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