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Ann. Geophys., 25, 1299-1310, 2007
www.ann-geophys.net/25/1299/2007/
© European Geosciences Union 2007
Recommendation for a set of solar EUV lines to be monitored for aeronomy applications
J. Lilensten1, T. Dudok de Wit2, P.-O. Amblard3, J. Aboudarham4, F. Auchère5, and M. Kretzschmar6
1LPG, CNRS and Joseph Fourier University, Bâtiment D de Physique, BP 53, 38041 Saint-Martin d'Hères cedex 9, France
2LPCE, CNRS and University of Orléans, 3A Avenue de la Recherche Scientifique, 45071 Orléans cedex 2, France
3LIS, CNRS, 961 Rue de la Houille Blanche, BP 46, 38402 St. Martin d'Hères cedex, France
4LESIA, Paris Observatory, 5 Place Jules Janssen, 92195 Meudon, France
5IAS, CNRS and Paris-Sud University, B�t. 121, 92405 Orsay cedex, France
6SIDC, Royal Observatory of Belgium, Avenue Circulaire 3, 1180 Brussels, Belgium
Abstract. In two recent studies, Dudok de Wit et al. (2005)
and Kretzschmar et al. (2006) have shown
that the solar Ultra-Violet spectrum between 25 and 195 nm can be
reconstructed from the observation of a set of 6 to 10 carefully chosen
spectral lines. The best set of lines, however, is application dependent. In
this study, we demonstrate that a good candidate for aeronomy applications
consists of the following 6 lines: H I at 102.572 nm, C III at 97.702 nm, O V at
62.973 nm, He I at 58.433 nm, Fe XV at 28.415 nm and He II at 30.378 nm. The TRANSCAR model is used to
quantify the impact of each individual line on the density, temperature and
velocity profiles. Using a multidimensional scaling technique, we show how to
select from this the best set of lines. Although this selection is motivated
by the specification of the ionosphere, our set of lines is also found to be
appropriate for reconstructing the variability of the solar spectrum between
25 and 195 nm.
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