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The atmosphere of Saturn's largest moon Titan is driven by photochemistry,charged particle precipitation from Saturn's upstream magnetosphere, andpresumably by the diffusion of the magnetospheric field into the outerionosphere, amongst other processes. Ion pickup, controlled by the upstreamconvection electric field, plays a role in the loss of this atmosphere. Theinteraction of Titan with Saturn's magnetosphere results in the formation of aflow-induced magnetosphere. The upstream magnetoplasma environment of Titan isa complex and highly variable system and significant quasi-periodic modulationsof the plasma in this region of Saturn's magnetosphere have been reported. Inthis paper we quantitatively investigate the effect of these quasi-periodicmodulations on the convection electric field at Titan. We show that theelectric field can be significantly perturbed away from the nominal radialorientation inferred from Voyager 1 observations, and demonstrate that upstreamcategorisation schemes must be used with care when undertaking quantitativestudies of Titan's magnetospheric interaction, particularly where assumptionsregarding the orientation of the convection electric field are made.

Electric field variability and classifications of Titan's magnetoplasma environment