Exploring solar wind drivers of omega bands

Omega bands are mesoscale auroral structures that emerge as eastward moving sinusoidal undulations of the poleward boundary of the equatorward oval in the post-midnight sector. They have been observed during the recovery phase of substorms and storms, and during periods of steady magnetospheric convection, but to date the statistical occurrence characteristics are unknown.

While omega bands can be seen during stormtime events, their drivers and the magnetospheric conditions in which they appear are not well understood. Gaining insight into the geomagnetic conditions and solar wind drivers that give rise to omega bands could greatly benefit theoretical and simulation studies, ultimately enhancing our understanding of global magnetospheric dynamics.  In this work, we perform a superposed epoch analysis of geomagnetic and solar wind parameters for omega band events identified using THEMIS ASI from 2006 to 2013. We use data from OMNI and SuperMAG to quantify the solar wind-magnetosphere-ionosphere system during these intervals. Since omega bands are known to have a near-Earth source, we hope to use this analysis to better understand their associated current systems and coupling mechanisms between the inner magnetosphere and ionosphere.