Theoretical Modelling of Chromospheric Emission Lines Through The Solar Activity Cycles 21–23 According To The Observational Analysis Results
Özet
In our previous papers, we compared the connection between the sizes
of faculae and plage regions, sunspots/sunspot groups (SGs), chromospheric
emission lines and solar spectral irradiance variability between the spectral
ranges 121.5–300.5 nm for the period 1981–2009 and discussed the changes in
the sunspot counts (SSCs) and the number of SGs relative to the variations in
solar activity indices. In this work, we tried to explain the theoretical reason
for these variabilities in the ultraviolet region and connected these changes to
the temporal variations of solar activity indices in comparison to different type
of SSCs/SGs for the first time in the literature. We found that the intensity of
Fe II (298.5 nm) ion in the last solar minimum was higher than the two previous
solar minima 21 and 22. So, the velocity of particles of Fe II ions increases
with decreasing density of the medium and increasing plage surface. Increasing
velocity causes an increase in the acceleration and intensity of particles.
