The High-Temperature Response of the TRACE 171 Å and 195 Å Channels

Details The High-Temperature Response of the TRACE 171 Å and 195 Å Channels The High-Temperature Response of the TRACE 171 Å and 195 Å Channels

Jun 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005apj...626.1110p&link_type=abstract

The Astrophysical Journal, Volume 626, Issue 2, pp. 1110-1115.

Astronomy and Astrophysics

Astronomy

14

Sun: Flares, Sun: Uv Radiation, Sun: X-Rays, Gamma Rays

Scientific paper

The CHIANTI spectral code is used to estimate line and continuum intensity contributions to the TRACE 171 and 195 Å channels, widely used for imaging a variety of solar features and phenomena, including quiet-Sun and active region loops and solar flares. It is shown that the 171 Å channel has a high-temperature response due to continuum and Fe XX line emission, so high-temperature (~10-20 MK) features in flares, prominent in TRACE 195 Å images as well as in X-ray images from Yohkoh and RHESSI, are sometimes visible in images made in the 171 Å channel. Such features consist of hot loop-top emission, either confined spots or ``spine'' structures in loop arcades. This is illustrated with TRACE and X-ray flare images.

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