The Temperature of the Bright Knots at the Tops of Solar Flare Loops

Details The Temperature of the Bright Knots at the Tops of Solar Flare Loops The Temperature of the Bright Knots at the Tops of Solar Flare Loops

Mar 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...459..773d&link_type=abstract

Astrophysical Journal v.459, p.773

Astronomy and Astrophysics

Astronomy

11

Magnetohydrodynamics: Mhd, Sun: Flares, Sun: Uv Radiation

Scientific paper

The Japanese Yohkoh spacecraft has revealed the pervasive presence of confined bright regions at the tops of solar flare magnetic flux tubes. The physical parameters in the bright regions, such as temperature and density, are of considerable interest for attempting to understand the nature and longevity of these regions. We have found an example of such a source in spectroheliograms of a flare observed by the Naval Research Laboratory slitless spectroheliograph on Skylab. This instrument offers better temperature discrimination than possible with a broadband X-ray telescope such as flown on Yohkoh We determine the temperature of the Skylab source using the most recent atomic data. From the Skylab extreme-ultraviolet images of this flare in spectral lines of Fe XXII, Fe XXIII, and Fe XXIV, we find that the confined bright region can be described as an isothermal source at a temperature of about 11 x 106 K. However, this conclusion generally contradicts temperatures measured from uncollimated Bragg crystal spectrometer spectra from Yohkoh and other spacecraft for similar X-ray class flares. There is also emission at the same location from Ca XVII ions formed at about 6 x 106 K, implying that the source might be multithermal A multithermal source would indicate that the bright regions are composed of structures below the spatial resolution of the Skylab and Yohkoh instrumentation and could possibly resolve the discrepancies between Bragg spectrometer and imaging data.

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