Relationship between the Coronal Activity and Magnetic Flux over Solar Cycle 24
Abstract
It is widely accepted that the variability of the solar white-light corona is closely connected to the solar activity. Many previous studies have revealed that the temporal variation of the total radiance of the K-corona follows the solar cycle pattern (e.g., correlated with sunspot number). However, systematic studies on the origin of the coronal mass and its variability are still rare. In this study, by means of the spherically symmetric inversion (SSI) method we reconstruct 3D coronal densities for Carrington Rotations (CRs) 2079--2180 over 2009--2017 using polarized brightness (pB) images observed with STEREO/COR1 and LASCO/C2. We calculate the total coronal mass from these density reconstructions within certain radial ranges, and compare its temporal evolution with the total magnetic flux measured from SOHO/MDI and SDO/HMI. We find a high correlation between the variations of total coronal mass and magnetic flux, and the former appears to be lagged by a CR to the latter during the rising phase of Cycle 24. To confirm this finding we also compare the observed coronal masses with those calculated from global thermodynamic MHD models by Predictive Science Inc (PSI), and compare the evolution of SDO/EVE line emissions between the chromosphere and the corona. In addition, we also explore the origin of the peaks in coronal mass and magnetic flux variations during the rising phase of Cycle 24.
- Publication:
-
2018 Triennial Earth-Sun Summit (TESS)
- Pub Date:
- May 2018
- Bibcode:
- 2018tess.conf10309W