Summary: 
The data and figures contained in this dataset are supporting materials for the paper referenced in the title and abstract below.  This study involved an analytical and numerical assessment of the Uranian magnetosphere and its interaction with the solar wind and interplanetary magnetic field (IMF). The data and figures contained in this dataset include supplementary results for a greater number of IMF orientations and Uranian seasons than the examples presented in the corresponding paper.

Abstract from corresponding paper: doi:10.1029/2023JA031791 with Journal of Geophysical Research Space Physics:
We investigate the unique magnetosphere of Uranus and its interaction with the solar wind. Following previous work, we developed and validated a simple yet valuable and illustrative model of Uranus’ offset, tilted, and rapidly-spinning magnetic field and magnetopause (nominal and fit to the Voyager-2 inbound crossing point) in three-dimensional space. With this model, we investigated details of the seasonal and interplanetary magnetic field (IMF) orientation dependencies of dayside and flank reconnection along the Uranian magnetopause. We found that anti-parallel (magnetic field shear angle greater than 170-degrees) reconnection occurs nearly continuously along the Uranian dayside and/or flank magnetopause under all seasons of the 84 (Earth) year Uranian orbit and the most likely IMF orientations. Such active and continuous driving of the Uranian magnetosphere should result in constant loading and unloading of the Uranian magnetotail, which may be further complicated and destabilized by sudden changes in the IMF orientation and solar wind conditions plus the reconfigurations from the rotation of Uranus itself. We demonstrate that unlike the other magnetospheric systems that are Dungey-cycle driven (i.e., Mercury and Earth) or rotationally driven (Jupiter and Saturn), global magnetospheric convection of plasma, magnetic flux, and energy flow may occur via three distinct cycles, two of which are unique to Uranus (and possibly also Neptune). Our simple model is also used to map signatures of dayside and flank reconnection down to the Uranian ionosphere, as a function of planetary latitude and longitude. Such mapping demonstrates that “spot”-like auroral features should be very common on the Uranian dayside, consistent with observations from Hubble Space Telescope. We further detail how the combination of Uranus’ rapid rotation and unique and very active global magnetospheric convection should be consistent with fueling of the surprisingly intense trapped radiation environment observed by Voyager-2 during its single flyby. Summarizing, Uranus is a very special magnetosphere that offers new insights on the nature, complexity, and diversity of planetary magnetospheric systems and the acceleration of particles in space plasmas, which might have important analogs to exoplanetary magnetospheric systems. Our hypotheses can be tested with further work involving more advanced models, new auroral observations, and unprecedented missions to explore the in situ environment from orbit around Uranus, which should include a complement of magnetospheric instruments in the payload. 

See the corresponding paper for description of the model that was used to generate these results. These movies and graphics and table all correspond to simulations of Uranus' interaction with the solar wind and estimates of reconnection along the dayside and flank magnetopause of the Uranian magnetosphere system. Also included are movies and graphics estimating auroral activity in the ionosphere at Uranus. All results are dependent on Uranian season (soltices, equinoxes, and mid-seasons), solar wind magnetic field vector (IMF), and diurnal (spin) phase. Also included are results supporting the validation of the model tested on Earth's magnetosphere. General descriptions of the various files are included in the README file.

The files and data contained here are in a series of figures (.pdf format), movies (.mp4 format), and excel spreadsheets.