Physics
Scientific paper
Jun 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995sowi.conf...30h&link_type=abstract
Observatoire de Paris-Meudon, International Solar Wind 8 Conference, p. 30
Physics
Type 3 Bursts, Solar Wind, Ulysses Mission, Solar Flares, Solar Electrons, Electron Acceleration, Radio Observation, Solar Corona, Radio Frequencies, Solar Wind Velocity
Scientific paper
Type 3 radio bursts allow us to follow energetic electrons ejected by solar flares into the interplanetary medium, even when the observer is far away from the electrons. The emission frequency fp is related to the ambient density ne by fp varies as the square root of ne, and as a function of the distance r to the sun we have approximately ne varies as r-2; as a consequence, on a 1/f - t dynamic spectrum type 3 bursts appear as nearly straight traces, whose slope gives an estimation of the source speed. We used the data of the URAP radio receiver on Ulysses (1-1000 kHz), observing sources in the solar wind, and the ground data of the ARTEMIS spectrograph (100-500 MHz), observing sources of the corona, over the years 1991-1994. We found a surprisingly large number of excellent high-frequency - low-frequency associations. A type 3 burst group on ARTEMIS (10 to 100 bursts over 1 to 10 minutes) typically gives rise to one isolated burst on Ulysses. As bursts often start in high frequencies during the maximum phase of flares, this demonstrates in a very convincing manner that some of the flare electrons themselves make it all the way to the interplanetary medium. We discuss decorrelation cases in the context of geometrical configuration between the active region and the two observing sites. We also study how apparent electron speeds vary with the distance to the sun.
Hoang Sang
Moncuquet Michel
Poquerusse M.
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