Magnetic topology of AR 11158 and morphology of its associated CMEs: Time evolution

F. A. IGLESIAS; CREMADES, H; C. H. MANDRINI

La Serena

Conferencia; Segunda reunion bincacional SOCHIAS-AAA; 2018

SOCHIAS y AAA

During days 13 to 16 of February 2011, corresponding to the rising phase of Solar Cycle 24, five class-M-or-higher flares and four CMEs originated at NOAA active region (AR) 11158. Due to the production of such a violent set of events and the rich multi-spacecraft data available, AR11158 has been the subject of multiple studies regarding the magnetic field topology evolution and mostly its correlation with the observed X-class flare properties (e.g. [1]-[5]). Additionally, [6] did a prelaminar study of the morphological properties of the ejected CMEs using the Graduated Cylindrical Shell model (GCS, see [7]) only at single instant of time when the CMEs are above a height of ~6 Rs. In this ongoing research we seek to obtain the coronal magnetic filed configuration above AR11158 using both linear and a non-linear force free extrapolations (LFFFE [8] and NLFFFE [9] respectively) of the photospheric fields during the whole time period under study, in order to derive the evolution of topological parameters associated to field instabilities. In addition, we estimate the time-evolution of the morphological properties of the ejected CMEs from the application of the GCS to several instants of time, including those where the CMEs are in the low corona, to study the correlation between the pre and post eruptive magnetic field configuration and the resulting CMEs? structure evolution.