Large-Scale Active Coronal Phenomena in Yohkoh SXT Images.
III. Enhanced Post-Flare Streamer

Center for Astrophysics and Space Sciences, UCSD, La Jolla, CA 92093–0424, U.S.A.

Frantisek Fárník
Astronomical Institute of Czech Academy of Sciences, 25165 Ondrejov, Czech Republic

Paul Hick
Center for Astrophysics and Space Sciences, UCSD, La Jolla, CA 92093–0424, U.S.A.

Hugh S. Hudson
Solar Physics Research Corporation, 4720 Calle Desecada, Tucson, AZ 85718, U.S.A.

Yutaka Uchida
Physics Department, Science University of Tokyo, 1–3 Kagurazaka, Shinjuku-ku, Tokyo 162, Japan

Abstract

We demonstrate several events where an eruptive flare close to the limb gave rise to a transient coronal streamer visible in X-rays in Yohkoh SXT images, and analyze one of these events, on 28–29 October 1992, in detail. A coronal helmet streamer began to appear 2 hours after the flare, high above rising post-flare loops; the streamer became progressively narrower, reaching its minimum width 7–12 hours after the flare, and widened again thereafter, until it eventually disappeared. Several other events behaved in a similar way. We suggest that the minimum width indicates the time when the streamer became fully developed. All the time the temperature in the helmet streamer structure was decreasing, which can explain the subsequent fictitious widening of the X-ray streamer. It is suggested that we may see here two systems of reconnection on widely different altitudes, one giving rise to the post-flare loops while the other creates (or re-forms) the coronal helmet streamer. A similar interpretation was suggested in 1990 by Kopp and Poletto for post-flare giant arches observed on board the SMM; indeed, there are some similarities between these post-flare helmet streamers and giant arches and, with the low spatial resolution of SMM instruments, it is possible that some helmet streamers could have been considered to be a kind of a giant arch.



ISSN 0038-0938