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How do solar activity proxies compare against the solar EUV spectral variability ?

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Abstract

For several decades, proxies for solar activity (such as the f10.7 and Mg II indices), rather than direct EUV measurements, have been used as inputs for ionosphere/thermosphere models. For that reason, it is important to quantify the capacity of each proxy to reproduce a given band of the EUV spectrum. Now that the EGS spectrograph onboard TIMED has been continuously operating for more than 6 years, it becomes possible to carry out a detailed comparison between solar proxies and various spectral lines, both on short and on long time-scales. Here, we use information theoretic criteria to quantify the amount of information that is shared between 9 proxies and a selection of important spectral lines. This analysis reveals in a synthetic way which proxies are most appropriate for reproducing specific spectral bands for modelling purposes, and how this can be interpreted in terms of physical processes on the Sun.
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Dates and versions

insu-00361507 , version 1 (16-02-2009)

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  • HAL Id : insu-00361507 , version 1

Cite

Thierry Dudok de Wit, Jean Lilensten, Matthieu Kretzschmar, J. Aboudarham. How do solar activity proxies compare against the solar EUV spectral variability ?. 37th COSPAR Scientific Assembly, Jul 2008, Montréal, Canada. ⟨insu-00361507⟩
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