Shape Parameters of 1991 to 2016 Solar Corona

Rhorom Priyatikanto

Published 2016-07-27Version 1

The global structure of solar corona observed in optical window is governed by the global magnetic field with different characteristics over solar activity cycle. Ludendorff flattening index becomes a popular measure of the global structure of solar corona as observed during eclipse. In this study, 15 digital images of solar corona from 1991 to 2016 were analyzed in order to construct the coronal flattening profiles as a function of radius. In most of the cases, the profile can be modeled with 2nd order polynomial function so that the radius with maximum flattening index ($R_{\text{max}}$) can be determined. Along with this value, Ludendorff index ($a+b$) was also calculated. Both Ludendorff index and $R_{\text{max}}$ show anti-correlation with monthly sunspot number, though the $R_{\text{max}}$ values are more scattered. The variation of $R_{\text{max}}$ can be regarded as the impact of changing coronal brightness profile over equator.