194. Rossby waves and the organization of photospheric magnetic fields
HMI magnetic field synoptic maps are used to evaluate the magnetic field structures’ organization and propagation as a function of time and latitude. It is demonstrated that the organization of longitudinal structures observed on synoptic maps is proportional to the level of activity at given latitudes.
193. Association Between Magnetic Pressure Difference and the Movement of Solar Pores
192. Magnetic helicity and free magnetic energy as tools for probing eruptions in two differently evolving solar active regions
An analysis of two active regions shows that differently evolving ARs may produce major eruptive flares even when, in addition to the accumulation of significant free magnetic energy budgets, they accumulate large amounts of both left- and right-handed helicity without a strong dominance of one handedness over the other.
191. Explaining why all solar cycles rise differently but decay in the same way
190. Improved CGEM Electric Field Inversion for HMI Active Regions
189. Spatial Scales and Time Variation of Solar Subsurface Convection
Spectral analysis of the spatial structure of solar subphotospheric convection is carried out for subsurface flow maps. It is found that the horizontal flow scales increase rapidly with depth, from supergranulation to giant-cell values. The total power of the convective flows is found to be anticorrelated with the sunspot number variation over the solar activity cycle in shallow subsurface layers and positively correlated at larger depths.
188. Constraining Global Solar Models through Helioseismic Analysis
Forward modeling is applied to numerous global hydrodynamic solar models, and helioseismic measurements on the meridional circulation are made using the forward modeling results. Comparison against the observational measurements shows significant differences, indicating our insufficient knowledge on either the global hydrodynamic modeling or the helioseismic inversions.