X-ray observations of a major eruptive flare behind the limb

Details X-ray observations of a major eruptive flare behind the limb X-ray observations of a major eruptive flare behind the limb

Feb 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994soph..149..363s&link_type=abstract

Solar Physics, vol. 149, no. 2, p. 363-380

Astronomy and Astrophysics

Astronomy

7

Coronal Loops, Emission Spectra, Radio Astronomy, Solar Corona, Solar Flares, Solar Spectra, Solar Temperature, Solar X-Rays, X Ray Astronomy, X Ray Imagery, Astronomical Spectroscopy, Goes 6, H Alpha Line, Skylab Program, Solar Limb, Solar Maximum Mission-A, Solar Radio Emission, X Ray Spectra, X Ray Spectroscopy

Scientific paper

We analyze X-ray images and spectra of a coronal structure which extended to altitudes over 130000 km above an eruptive flare located 20 deg behind the western solar limb. The images were obtained by the Flat Crystal Spectrometer (FCS) and the spectra were obtained by the Bent Crystal Spectrometer (BCS) aboard the SMM spacecraft. Images in O VIII and Mg XI lines cover the period from before the flare onset (which occurred at 22:31 UT on 16 February, 1986) through 17 UT on 17 February and were used for determination of temperature and emission measure within the structure. BCS obtained Ca XIX spectra of the coronal event, benefiting from the occultation of the active region behind the solar limb. The BCS data show, and FCS data confirm, that the temperature, after an initial rise and decline, stayed almost constant for many hours after 04:30 UT on 17 February. This may indicate that initially we observed the rise and decay of post-flare loops, but later the X-ray emission came predominantly from a post-flare giant arch that formed above them. This has been observed in many previous cases. However, a comparison with other events characterized by very high post-flare loops suggests that we may be observing the same system of slowly growing groups all the time. Therefore, we suggest a third possibility, i.e., that such anomalously high loop systems first behave like post-flare loops but gradually take over some characteristics of a post-flare giant arch. The Soft X-ray Telescope aboard Yohkoh, with spatial resolution improved by nearly an order of magnitude, might be able to check up on the development of such large-scale coronal structures if proper observational modes are applied after the occurrence of major eruptive flares.

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