Energization Mechanisms Leading to Vertical Ion Transport in Jupiter's Auroral Region Ionosphere

Energization and escape of ionospheric plasma is known to occur at Jupiter, with Juno/JEDI observations of ion conics by Clark et al. [2017] indicating wave heating and escape of ions from Jupiter's ionosphere, as well as Galileo and New Horizons observations of ionospheric-origin H2+ and H3+ in the magnetosphere [Hamilton, 1980 and Nicolaou et al., 2015]. The escape of plasma from Jupiter requires a confluence of energization and transport mechanisms, including ionization, electron heating through the transfer of heat flux from the magnetosphere and low-energy particle precipitation, and ion heating by low-energy particle precipitation and wave-particle interactions. We show the effects and interaction of these processes on magnetic field-aligned ion transport using the Polar Wind Outflow Model (PWOM). For this study, PWOM is coupled with the Jupiter Global Ionosphere-Thermosphere Model (J-GITM) and a two-stream model of superthermal electrons (GLobal airglOW, or GLOW). We use both a multi-fluid version of PWOM that includes ionization and precipitation effects, and a fluid-kinetic version that includes wave-particle interactions at high altitudes. We place the results in the context of published Juno data and discuss the influence of observed magnetospheric drivers on vertical ion transport that may lead to escape of ionospheric plasma.