G. V. Yakunina
Articles written in Journal of Astrophysics and Astronomy
Volume 9 Issue 1 March 1988 pp 41-47
Using the line profiles of [Fe x] 6374 å and [Fe XIV] 5303 å emission lines observed during five total solar eclipses, we address the problem whether the solar corona is static or contains moving features. Many of the profiles of both emission lines have complicated shapes, which we interpret as an evidence for the existence of many, small, moving features in the corona. The line-of-sight velocities observed by other investigators (
Volume 9 Issue 2 June 1988 pp 125-125 Erratum
Volume 35 Issue 1 March 2014 pp 1-15 General Editorial on Publication Ethics
The correlation coefficients of the linear regression of six solar indices versus 10.7 cm radio flux 𝐹10.7 were analysed in solar cycles 21, 22 and 23. We also analysed the interconnection between these indices and 𝐹10.7 with help of approximation by polynomials of second order. The indices we have studied in this paper are: the relative sunspot numbers – SSN, 530.3 nm coronal line flux – 𝐹530 , the total solar irradiance – TSI, Mg II 280 nm core-to-wing ratio UV-index, the Flare Index – FI and the counts of flares. In most cases the regressions of these solar indices vs. 𝐹10.7 are close to the linear regression except the moments of time near the minimums and maximums of the 11-year activity. For the linear regressions, we found that correlation coefficients 𝐾corr(𝑡) for the solar indices vs. 𝐹10.7 and SSN dropped to their minimum values twice during each 11-year cycle.
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