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29 July 2010 It's time for a new EUV orbital mission
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The EUV waveband includes critical spectral features containing diagnostic information often not available at other wavelengths, and the bulk of radiation from million degree plasmas is emitted in the EUV. Such plasmas are ubiquitous, and examples include white dwarf photospheres; accretion phenomena in young stars, CVs and AGN; stellar coronae; and the ISM of our galaxy and of others. However, sensitive high-resolution spectroscopy is required to resolve and identify source and ISM spectral features unambiguously, and to measure line profiles and Doppler shifts. This allows exploitation of the full range of plasma diagnostic techniques developed in laboratory and solar physics. The J-PEX high-resolution EUV spectrometer has made a breakthrough in capability with an effective area of 7 cm2 (220-250 Å) and resolving power of 4000, which exceed EUVE by factors of 7 and 20 respectively, and cover a range beyond the 170-Å cutoff of the Chandra LETG. J-PEX has flown successfully twice on NASA sounding rockets, but NASA has approved no new orbital EUV mission. It is time for one. Here we describe the scientific case for high-resolution EUV spectroscopy, summarize the technology that makes practical such measurements, and present concepts for a ~3-month orbital mission and for larger missions.
© (2010) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.
M. P. Kowalski, K. S. Wood, M. A. Barstow, and R. G. Cruddace "It's time for a new EUV orbital mission", Proc. SPIE 7732, Space Telescopes and Instrumentation 2010: Ultraviolet to Gamma Ray, 77322E (29 July 2010);

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