Dissimilarity in the evolution of solar EUV and solar radio emission (2800 MHz) during 1999-2002

Details Dissimilarity in the evolution of solar EUV and solar radio emission (2800 MHz) during 1999-2002 Dissimilarity in the evolution of solar EUV and solar radio emission (2800 MHz) during 1999-2002

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003jgra..108.1455k&link_type=abstract

Journal of Geophysical Research, Volume 108, Issue A12, pp. SSH 9-1, CiteID 1455, DOI 10.1029/2003JA009869

Astronomy and Astrophysics

Astrophysics

1

Solar Physics, Astrophysics, And Astronomy: Solar And Stellar Variability, And Astronomy: Chromosphere, And Astronomy: Corona, And Astronomy: Photosphere, And Astronomy: Radio Emissions

Scientific paper

For solar UV and EUV the F10 (2800 MHZ solar radio emission), Lyman alpha, and Mg II are used as proxies. During 1999-2002, many solar indices showed two maxima, one near July 2000 and another near January 2002. For F10 and Lyman alpha, the second maximum was higher than the first maximum by ~10%, but for Rz, the second maximum was lower than the first maximum by ~4%. The observed EUV (26-34 nm from SEM-SOHO) had the second maximum higher than the first maximum, but only by ~3.5%. The model values given in SOLAR2000 [Tobiska et al., 2000] show patterns of 26-34 nm qualitatively similar to F10, with second maximum larger than the first maximum, but the magnitude is much larger, ~20%. Thus there is a discrepancy of ~15% between observed EUV and SOLAR2000 model EUV during 2001-2002. The model values are overestimates and do not seem to have taken into account the observed EUV values.

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