Modelling 1-D quasi-static potential structures at Jupiter

<p>Quasi-static potentials have long thought to be one of the significant drivers of the main ultraviolet emission associated with Jupiter&#8217;s auroral oval. The magnetic field lines connecting to the auroral zone extend into Jupiter&#8217;s middle magnetosphere, at radii of 20R_J &#8211; 50 R_J. Such quasi-static potential structures are capable of accelerating charged particles into the planetary ionosphere and generating aurora, with the Juno JEDI instrument observing inverted-V potential structures on the order of megavolts. However, Juno&#8217;s observation of quasi-static potentials has not been as ubiquitous as was initially theorised. Juno has observed more frequent instances of bi-directional electron beams on the same field line, indicating the presence of dynamic processes occurring at different altitudes. In addition, this suggests that quasi-static potentials may not be a significant driver for the main UV emission.</p><p>&#160;</p><p>In this paper, we present new results from a 1-D Vlasov model of the high-latitude magnetic field lines in the Jovian mid-magnetosphere. Our model is time-dependent and features a non-uniform mesh close to the ionosphere, allowing us to examine the formation of quasi-static potential structures in the upward current region over the course of a simulation. We will also present simulations showing the collapse and reformation of these potential structures, with the collapse showing the propagation of electron beams in both directions along the modelled field line.</p>