Hard X-Radiation from a Fast Coronal Ejection

Details Hard X-Radiation from a Fast Coronal Ejection Hard X-Radiation from a Fast Coronal Ejection

Nov 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001apj...561l.211h&link_type=abstract

The Astrophysical Journal, Volume 561, Issue 2, pp. L211-L214.

Astronomy and Astrophysics

Astronomy

37

Sun: Corona, Sun: Flares, Sun: X-Rays, Gamma Rays

Scientific paper

We have observed a high-speed coronal ejection in hard X-rays, detectable to an altitude of some 2×105 km in the Yohkoh 23-53 keV energy bands. Simultaneous imaging at 17 and 34 GHz from the Nobeyama radioheliograph shows complex moving features simultaneous with the ejection, including a compact source that we identify with the rapid X-ray source motion. The hard X-ray and microwave observations agree on ejection velocities in the vicinity of 1000 km s-1. The hard X-ray sources also corresponded in position angle to a bright coronal mass ejection (CME) detected about 15 minutes later and temporally to both fast-drift and slow-drift radio bursts in the decimeter-meter bands. Other components of coronal hard X-ray emission were also detected, including an extended long-duration event with a nonthermal spectrum. We suggest that a major eruptive flare occurred in NOAA Active Region 9415, approximately 26° beyond the west limb at the time of the event. Estimating a source density of 4×109 cm-3 from the compact source observed at 17 GHz, we find a total electron number (>20 keV) of approximately N20~1.3×1036 for the compact part of the source. We infer that these electrons were trapped in expanding loops forming a part of the CME and may have contributed substantial pressure within these loops.

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