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R.A. Harrison (Space Science Dept., Rutherford Appleton Laboratory)
Studies of the extreme ultraviolet (EUV) and ultraviolet (UV) spectrum of the Sun provide a unique and powerful means to investigate plasma properties, such as density, temperature, abundance and flow speeds throughout the low solar atmosphere, from chromsphere to corona. In particular, with the SOHO mission, recent EUV/UV spectroscopic studies have paved the way for significant advances in numerous areas of solar physics research, such as active region structure and evolution, quiet Sun transient processes, mass ejection onset, and so on... and the wealth of data will guarantee that we will be reaping the rewards for some time to come. However, spectroscopy demands relatively high mass, high telemetry instrumentation, and the products are not readily understood by the non-specialist. Thus, with the new breed of lighter missions and a greater need to enhance public awareness, what is the future for solar EUV/UV spectroscopy? The NASA STEREO mission due for launch in 2004 is not expected to carry a spectrometer. The Japanese Solar-B mission will be carrying an EUV spectrometer. The need for such instruments for the possible ESA Solar Orbiter, the NASA Solar Probe and other future missions must be addressed. SOHO comes from mid-1980's technology so we can readily enhance our current performances with the use of multilayers, improved CCD technology, multi-line-of-sight observations etc... So, as well as advertising the success of solar spectroscopy in recent years, an outline of possible directions willl be given which will underline the strong case for including such experiments in future solar missions.
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