Mapping Jupiter’s Lyman-α Airglow with Juno UVS

Jupiter’s low latitude upper atmosphere is a region with notable airglow emissions. We can view these emissions using Juno’s UltraViolet Spectrograph (UVS). A major component of Jupiter’s far-utraviolet airglow is from Lyman alpha (Lyα) emissions largely caused by scattering of solar Lyα light off H atoms in Jupiter’s thermosphere. Juno’s low altitude ( 3500 km above the 1-bar level) perijoves allow UVS to detect hydrogen Lyα emissions in all directions, and to create maps that inform us about the
vertical structure of Jupiter’s upper atmosphere. We present preliminary results to characterize these emissions and how they vary with respect to spacecraft latitude, longitude, zenith angle, and local time information. We will use the results from many perijove passes to model the atmosphere and determine properties about the population of hydrogen that we find in Jupiter’s low latitudes.