Modeling Solar Atmospheric Phenomena with AtomDB and PyAtomDB

Taking advantage of the modeling tools made available by PyAtomDB Foster(2015), we eval- uated the atomic impact of solar phenomena. In particular, the atomic effects of coronal mass ejections (CME). Intitially, we perform modifications to the canonical SunNEI code N.A.Murphy et al.(2011) in order to include non-equilibrium ionization (NEI) processes that occur in the CME modeled in SunNEI. The methods used involve the consideration of radiaitive cooling as well as ion balance calculations produced by PyAtomDB. These calculations were subsequently implemented within the SunNEI simulation. The insertion of aforementioned processes and parameter customizaton produced quite similar results of the original model aside from the inconsistencies between the Fe charge states, which we found to stem from incongruent data for Argon-like Fe ions between the CHIANTI and AtomDB databases. The key finding was that theoretical models are greatly impacted by the relative atomic database update cycles. We then use the AtomDB databsase to model the time depedencies of intensity flux spikes produced by a coronal shock wave Ma et al.(2011). Having the data provided al- lowed us to produce a theretical representation that interpolated over the intensity data points for each respective Astronomical Imaging Assembly (AIA) wavelength band pass. Specifically, the 171 Å (Fe IX) ,193 Å (Fe XII, FeXXIV),211 Å (Fe XIV), and 335 Å (Fe XVI) wavelengths in or- der to assess the comparative spectral emissions between AtomDB and the observed data. The results of the theoretical model, in principle, should shine light in regards to the equilibrium conditions related to the precipitant ionic abundances present within the shock front, which will allow for better undertsanding of energy jumps as well as atomic variabilities at play in the shock wave.