Line Profile Studies of Coronal Active Regions in Fe XII {\lambda}195.12 Using Hinode/EIS

TL;DR

This study analyzes Fe XII line profiles in coronal active regions over two solar cycles using Hinode/EIS data, revealing variations in line parameters and their relation to solar activity, with implications for coronal heating.

Contribution

It provides a comprehensive analysis of line profile variations in active regions across solar cycles, introducing multicomponent line profile modeling to explain observed behaviors.

Findings

Doppler velocity and centroid exhibit six different behaviors relative to rest wavelength.

Centroid shifts are more prominent than Doppler velocity shifts.

Line width correlates with intensity and varies with the solar cycle.

Abstract

Coronal active regions are studied using Hinode/EIS observations in the EUV line Fe XII {\lambda}195.12 by analyzing their line profiles from 2006 December to 2019 December. The period covers the last 2 yr of solar cycle 23 and solar cycle 24 fully. Active regions are the main source of magnetic field in the solar atmosphere, important in its heating and dynamics. Line profiles were obtained from various active regions spread across the Sun on a monthly basis from which we obtained the intensity, line width, Doppler velocity, and centroid and examined their variation during the solar cycle. The histograms of the Doppler velocity and centroid show that they behave in six different ways with respect to the position of rest wavelength. In addition, the shifts in the centroid were found to be more compared to the Doppler velocity. The variation of the line width with respect to the Doppler velocity or the centroid mostly follows a second-degree polynomial. A multicomponent line profile is simulated to explain the difference in the behavior of the Doppler velocity and the centroid with respect to the line width. We also find that the intensity and the line width of the different data sets show a global dependence on the solar cycle with a good correlation. The implications of the results for the coronal heating and dynamics are pointed out.