Far-side imaging tools, front-side imaging, and EUV solar irradiance forecasting

Details Far-side imaging tools, front-side imaging, and EUV solar irradiance forecasting Far-side imaging tools, front-side imaging, and EUV solar irradiance forecasting

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh12a..03f&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH12A-03

Astronomy and Astrophysics

Astrophysics

[7549] Solar Physics, Astrophysics, And Astronomy / Ultraviolet Emissions, [7924] Space Weather / Forecasting, [7969] Space Weather / Satellite Drag

Scientific paper

Currently we are in an advanced stage of the development of an application of both far-side and front-side imaging to EUV solar irradiance forecast. The basic method and its application to one case were described by Fontenla et al. (2009). This method uses a combination of several techniques for far-side imaging with front-side images at various wavelengths, and EUV spectral synthesis. This presentation shows that all these techniques should be used in concert to produce a reasonably accurate EUV irradiance forecast at Earth and other planets. The combination of SOHO/SWAN Ly alpha backscattering, far-side helioseismic images, and front-side imaging resolves the weaknesses of each technique by itself. In particular, the presentation will show how the SOHO/SWAN data plays a very important role in this combination by supplying unique EUV data (Ly alpha) that is not directly inferred by helioseismic methods. The SOHO/SWAN data plays a key role in the combination by allowing us to infer the evolution in EUV brightness of the active regions on the far-side of the Sun. However, because this method does not provide a good localization of the emission sources in the Sun, it needs to me complemented by the good localization that helioseismology provides. Because the Ly alpha backscattering is sensitive to active network and plage these images provide essential information for determining the far-side evolution of components to the solar flux that are not detected by helioseismology but have important effects on the EUV irradiance. However, again because of the poor localization of these features in backscattering images, front side imaging is also a necessary complement that helps in the localization on the solar surface of the changes observed in the SOHO/SWAN images.

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