Ulysses-ARTEMIS radio observation of energetic flare electrons

Details Ulysses-ARTEMIS radio observation of energetic flare electrons Ulysses-ARTEMIS radio observation of energetic flare electrons

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aipc..382...62p&link_type=abstract

Proceedings of the eigth international solar wind conference: Solar wind eight. AIP Conference Proceedings, Volume 382, pp. 62-

Physics

4

Particle Emission, Solar Wind, Radio, Microwave

Scientific paper

We used type III radio bursts recorded by the ARTEMIS spectrograph on the ground (100-500 MHz), and by the URAP radio receiver on the Ulysses spacecraft (1-940 kHz), to follow energetic electrons ejected from solar flares into the interplanetary medium (IPM). Out of about 200 large events observed over 1991 1994, we found ~50% frequency associations. Typically, a group of many bursts on ARTEMIS gives rise to one isolated burst on Ulysses. This demonstrates that some of the flare electrons themselves make it all the way to the IPM. We confirm that speeds deduced from frequency drifts are ~c/3 in the corona and c/10 in the IPM. We find that this deceleration occurs before about 0.1 AU, and that there is no significant correlation between the initial and final speeds. We derive the average radiation pattern of type III bursts at low frequencies and find that the maximum intensity direction is shifted ~40° east of the radial direction, which we interpret as resulting from an ambient density gradient directed in the opposite direction. We suggest that right above ``open'' coronal magnetic field lines imbedded inside active regions, the solar wind presents a local maximum speed; then interaction with the relatively slower wind around results in a westward density gradient.

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