Abstract/Summary

Recently, H₃⁺ was detected at Saturn’s low- and mid-latitudes for the first time (O’Donoghue et al. [2013]. Nature 496(7444), 193–195), revealing significant latitudinal structure in H₃⁺ emissions, with local extrema in one hemisphere mirrored at magnetically conjugate latitudes in the opposite hemisphere. The observed minima and maxima were shown to map to regions of increased or decreased density in Saturn’s rings, implying a direct ring–atmosphere connection. Here, using the Saturn Thermosphere Ionosphere Model (STIM), we investigate the “ring rain” explanation of the O’Donoghue et al. (2013) observations, wherein charged water group particles from the rings are guided by magnetic field lines as they “rain” down upon the atmosphere, altering local ionospheric chemistry. Based on model reproductions of observed H₃⁺ variations, we derive maximum water influxes of (1.6–16) × 10⁵ H₂O molecules cm⁻² s⁻¹ across ring rain latitudes (approximately 23–49° in the south, and approximately 32–54° in the north), with localized regions of enhanced influx near 48°, 38°, 42°, and 53° latitude. We estimate the globally averaged maximum ring-derived water influx to be (1.6–12) × 10⁵ cm⁻² s⁻¹, which represents a maximum total global influx of water from Saturn’s rings to its atmosphere of (1.0–6.8) × 10²⁶ s⁻¹. The wide range of global water influx estimates stems primarily from uncertainties regarding H₃⁺ temperatures (and consequently column densities). Future ring rain observations may therefore be able to reduce these uncertainties by determining H₃⁺ temperatures self-consistently.