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Temperature Response of the 171 Å Passband of the SWAP Imager on PROBA2, with a Comparison to TRACE, SOHO, STEREO, and SDO
Raftery, Claire L.; Bloomfield, D. Shaun; Gallagher, Peter T.; Seaton, Daniel B.; Berghmans, David; De Groof, Anik
AA(Space Sciences Laboratory, UC Berkeley; Astrophysics Research Group, School of Physics, Trinity College Dublin), AB(Astrophysics Research Group, School of Physics, Trinity College Dublin), AC(Astrophysics Research Group, School of Physics, Trinity College Dublin), AD(Solar Physics, Royal Observatory of Belgium), AE(Solar Physics, Royal Observatory of Belgium), AF(Solar Physics, Royal Observatory of Belgium)
Solar Physics, Volume 286, Issue 1, pp.111-124 (SoPh Homepage)
Publication Date:
Corona, Flares, spectrum, Instrumental effects, Spectrum, ultraviolet
Abstract Copyright:
(c) 2013: Springer Science+Business Media Dordrecht
Bibliographic Code:


We calculated the temperature response of the 171 Å passbands of the Sun Watcher using APS detectors and image Processing (SWAP) instrument onboard the PRoject for OnBoard Autonomy 2 (PROBA2) satellite. These results were compared to the temperature responses of the Extreme Ultraviolet Imaging Telescope (EIT) onboard the Solar and Heliospheric Observatory (SOHO), the Transition Region and Coronal Explorer (TRACE), the twin Extreme Ultraviolet Imagers (EUVI) onboard the Solar TErrestrial RElations Observatory (STEREO) A and B spacecraft, and the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO). Multiplying the wavelength-response functions for each instrument by a series of isothermal synthetic spectra and integrating over the range 165 - 195 Å produced temperature-response functions for the six instruments. Each temperature response was then multiplied by sample differential emission-measure functions for four different solar conditions. For any given plasma condition ( e.g. quiet Sun, active region), it was found that the overall variation with temperature agreed remarkably well across the six instruments, although the wavelength responses for each instrument have some distinctly different features. Deviations were observed, however, when we compared the response of any one instrument to different solar conditions, particularly for the case of solar flares.
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