*********************************
There is now a CONTENT FREEZE for Mercury while we switch to a new platform. It began on Friday, March 10 at 6pm and will end on Wednesday, March 15 at noon. No new content can be created during this time, but all material in the system as of the beginning of the freeze will be migrated to the new platform, including users and groups. Functionally the new site is identical to the old one. webteam@gatech.edu
*********************************
The defense will be held on October 19th at 12:15 pm in ES&T 1129. For more information, please see attachment.
Title: Diurnal and Seasonal Variability of Uranus’ Magnetosphere under Different IMF
Committee members: Dr. Carol Paty ( Advisor), Dr. Zhigang Peng, Dr. James Wray, Dr. Paul Steffes, Dr. Mitchell Walker
Abstract: The magnetosphere of Uranus is far from well known since there was only one fly-by measurement in history. In order to study the magnetosphere and its coupling mechanism with the solar wind, we used our multifluid magnetohydrodynamics (MHD) model [Cao and Paty, 2017] to successfully simulate the variation of the global magnetosphere of Uranus and have predicted potential favorable reconnection locations. We proposed that a “switch-like” magnetosphere exists at Uranus in both equinox and solstice seasons, where the planetary rotation drives the interchange between an open magnetosphere and a closed magnetosphere each Uranus day. This periodic reconnection is predicted to occur upstream of the magnetopause, with a frequency that corresponds to the planetary rotation (once per 17.24 h). The locations of the bow shock and magnetopause in our model are validated against measurements made by Voyager 2. In examining the evolution of the magnetic field configuration along with that of high plasma beta regions, which in combination indicate where the system is favorable for reconnection, we found that the reconnection that occurs is highly dependent on the rotation of the planetary magnetic field in both equinox and solstice seasons. These periodic reconnection events in our simulation support our hypothesis of a periodic “switch-like” magnetosphere at Uranus. We then investigated the diurnal and seasonal variations of the magnetopause boundary under different Interplanetary Magnetic Field (IMF) orientations, combined with Voyager 2’s measurement. We quantitatively analyzed the characteristics and variability of Uranus’ magnetopause and cusp in terms of the subsolar’s standoff distance, the flaring parameter and the cusp indentation, which give us an initial intuition of the asymmetric structure of the magnetopause. Our results show that the asymmetry of the magnetopause is highly dependent on the rotation of Uranus under specific IMF orientations. The shape of the magnetopause is also affected by the off-centered dipole moment. Our model can be applied to other planets with different magnetic geometries, such as the exoplanets and the Neptune-Triton system.
