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

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.