EUV coronal pattern of complexes of solar activity

Studying of the coronal plasma associated with long-lived complexes of the solar activity is important for understanding a relationship between the magnetic activity and the solar corona changing during the solar cycle.

In the present paper, two long-lived complexes of the solar activity at the beginning of the current solar cycle 23 are investigated by using the Extreme-Ultraviolet data (EUV) from SOHO/EIT. For this purpose the EIT limb synoptic maps during the CR1916–CR1919 (11 November 1996–1 March 1997) are obtained.

The coronal temperature structures derived from the three lines 171A (Fe IX,X), 195A (Fe XII)and 284A (Fe XV) are investigated by applying an algorithm developed by Zhang et al. [Zhang, J., White, S.M., Kundu, M.R. ApJ 527, 977, 1999]. Standard EIT software are used for the temperature estimation from the ratio of two lines of Fe IX,X and Fe XII.

The method of the rotational tomography with a correction for an inclination of the Earth’s orbit (B-angle) to the helioequator is applied to obtain the three-dimensional (3-D) coronal structure of the complex of the solar activity. The results reveal difference in temperature structures related to multi-poles magnetic structures of the complex of solar activity and to the typical, the bipolar activity complex.