Würzburg 2018 – wissenschaftliches Programm
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EP: Fachverband Extraterrestrische Physik
EP 3: Sun and Heliosphere I - Structure (MHD, Corona, TR, SW-acc.-Region)
EP 3.3: Vortrag
Dienstag, 20. März 2018, 17:15–17:30, BSZ - Pabel HS
Coronal magnetic field evolution over the cycle 24 — •Iulia Chifu1,2, Thomas Wiegelmann1, and Bernd Inhester1 — 1Max Planck Institute for Solar System Research,Goettingen,Germany — 2Astronomical Institute of Romanian Academy, Bucharest,Romania
Many explosive phenomena, like flares and coronal mass ejections are caused by instabilities in the solar corona. Most of the time there is a strong correlation between the eruptive events and the evolution of the magnetic field. The low density and magnetic field intensity in the solar corona makes it difficult to obtain direct measurements of the magnetic field. We therefore extrapolate photospheric synoptic vector magnetograms from SDO/HMI into the corona. We use the nonlinear optimization method to reconstructed the magnetic field over the cycle 24, assuming that a force-free coronal magnetic field. We analyse this 10-year data set regarding the evolution of the free magnetic energy, correlation with the global flaring activity. We investigate also the location and structure of open field regions (coronal holes) and their separatrices to closed helmet streamer like regions.