Analyzing Constraints on Coronal Jets Near Filaments and Sigmoidal Active Regions Using Nonlinear Force-Free Models

Throughout the eleven year cycle of the sun, solar eruptions are constantly taking place. Thought to be caused by reconnection of magnetic field lines, coronal jets are one of several types of such eruptions. Jet formation and eruption is not well understood. In some cases, jets occur when small filaments of chromospheric material are lofted into the corona. The filaments have strong magnetic flux, and are often the site of magnetic reconnection and subsequent eruption. In order to better understand the constraints on these coronal jets, we have modeled the conditions required for stable filaments and eruptions using nonlinear force-free (NLFF) field modeling. NLFF models are 3-D topological models that are used to show the morphological evolution of magnetic fields. Using the CMS2 modeling suite, we modeled two regions with jet eruptions: a coronal jet near a larger filament, and a coronal jet near an AR sigmoid. In both cases, Solar Dynamics Observatory’s HMI magnetograms and observations from AIA images are used to constrain the input parameters of the model. In this presentation, we will present our model results and discuss how they help understand solar coronal jet eruptions.This work is supported by NSF-REU solar physics program at SAO, grant number AGS-1560313, and NASA grant number NNX15AF43G