Ion Upflow Dependence on Ionospheric Density and Solar Photoionization

Abstract:

Wahlund et al. [1992] first categorized the upflow of ionospheric ions into two types: that driven by ion frictional heating and that caused by auroral precipitation. Motivated by rocket observations showing a variety of different ionospheric responses to precipitation, this paper explores the influence of the background ionospheric density on upflow resulting from auroral precipitation. Simulations of upflow driven by auroral precipitation were conducted using a version of the Varney et al. [2014] model driven by precipitation characterized by observations made during the 2012 Magnetosphere-Ionosphere Coupling in the Alfvén resonator (MICA) rocket mission and using a variety of different initial electron density profiles. The simulation results show that increased initial density before the onset of precipitation leads to smaller electron temperature increases, longer ionospheric heating timescales, weaker ambipolar electric fields, lower upflow speeds, longer upflow timescales, but larger upflow fluxes. The upflow flux can increase even when the ambipolar electric field strength decreases due to the larger number of ions that are accelerated. Long-term observations from the European Incoherent Scatter (EISCAT) Svalbard radar taken during the International Polar Year (IPY) support the effects seen in the simulations. This correlation between ionospheric density and ion upflows emphasizes the important role of photoionization from solar ultraviolet radiation, which the EISCAT observations show can increase ionospheric density by as much as an order of magnitude during the summer months.