Abstract
Our knowledge of the the solar atmosphere comes from the light analysis. The ultraviolet wavelength is the privileged spectral range to study the solar plasma in several stages of ionization emitted from the chromosphere to the corona. Starting with basic notions of spectroscopy, an overview of important parameters is given. Then, after a short description of classical spectrometers, a detailed analysis of the properties of the mountings used on SOHO is performed; some examples are shown. I discuss how to separate the real solar signal from the instrumental contribution.
From what has been learnt on the Sun during the last two decades, I make a prospective for future solar spectrometers developments.
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Lemaire, P. (1998). Instrumentation: Spectroscopy. In: Vial, J.C., Bocchialini, K., Boumier, P. (eds) Space Solar Physics. Lecture Notes in Physics, vol 507. Springer, Berlin, Heidelberg. https://doi.org/10.1007/BFb0106923
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DOI: https://doi.org/10.1007/BFb0106923
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