Effects of Energetic O+ Outflow on the Inner Magnetosphere During Superstorms

The increasing interest in attaining space weather prediction capabilities inevitably leads to a consolidated study of the solar wind-magnetosphere-ionosphere system. A key piece consists of understanding the transport of energy and particles between the different regions and under different geomagnetic conditions. Extreme geomagnetic storms have been the subject of special attention, not only due to their harmful effects on the human presence in space and on ground-based technologies, but also because under such conditions kinetic effects can reach global scales. One such effect has been observed by satellite missions after interplanetary shock impacts leading to superstorms. In situ measurements show that O⁺ ions can outflow from the ionosphere and be energized to energies in the range of keV and tens of keV. This study examines the effects of outflowing energetic ions on the inner magnetosphere using the Comprehensive Inner Magnetosphere Ionosphere (CIMI) model. The modeling work aims to determine the extent of energization that the outflowing ions undergo and their path into the magnetosphere. Special attention is paid to the path followed by the ions to establish if they can access the ring current region directly instead of outflowing to the tail plasma sheet, as conventionally thought, and the implications of such ionospheric source in the development of the storm-time ring current.