Using FUV remote-sensing methods to investigate solar EUV variability with the aid of TIMED/GUVI observations

Details Using FUV remote-sensing methods to investigate solar EUV variability with the aid of TIMED/GUVI observations Using FUV remote-sensing methods to investigate solar EUV variability with the aid of TIMED/GUVI observations

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsa33b1767c&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SA33B-1767

Astronomy and Astrophysics

Astrophysics

[0310] Atmospheric Composition And Structure / Airglow And Aurora, [7519] Solar Physics, Astrophysics, And Astronomy / Flares, [7538] Solar Physics, Astrophysics, And Astronomy / Solar Irradiance, [7974] Space Weather / Solar Effects

Scientific paper

In a 2007 JGR paper, Strickland et al. presented a remote-sensing method for specifying solar EUV spectra shortward of 45 nm and applied it to two intense flare events which occurred in late 2003. The method uses spectral irradiances from TIMED/SEE longward of 27 nm, values shortward of 5 nm based on a scaling algorithm applied to time-coincident GOES/XRS 0.1-0.8 nm data, and time-coincident TIMED/GUVI observations which specify values between 5 and 27 nm. Validation was carried out by comparing derived electron density profiles (using derived flare and preflare EUV spectra) with observed profiles. Here, we address recent results which extend the work reported in 2007. A brief discussion will be given to extensive software revisions implemented for the purpose of conveniently utilizing data over multiple solar rotations from the above instruments. A list of 2002-2005 X-class flares will be included from a XRS-based survey for which good observations were made by SEE and GUVI. New results will be presented in the form of spectra and integrated solar energy fluxes, namely QEUV in units of mW m-2. Of particular interest is how well our derived spectra and corresponding QEUV values agree with Version 10.02 SEE measurements. Results to date beyond those reported in 2007 show agreement in non-flare QEUV values to within ~15% while for flares, somewhat less agreement to ~30%. This shows a significant improvement over the 2007 comparisons with Version 8 SEE data. We also specify GUVI-based QEUV using a lookup table method which works well under non-flare conditions. For QEUV values using this approach, comparisons will be made with SEE over multiple solar rotations which further demonstrate the effectiveness of FUV remote sensing for addressing EUV variability.

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