Comparison of Sub-proton Scale Magnetic Holes in the Magnetosheath, Magnetotail, and Foreshock

Magnetic holes are frequently observed throughout Earth's magnetosphere, but there is still much about them that is not understood. Magnetic holes are characterized by a local depression in magnetic field strength caused by current vortices. These current vortices can be carried by electrons or ions, but the electron driven, or sub-proton scale magnetic holes are seemingly the most abundant. Despite the abundance of these magnetic holes, we have only recently been able to observe them due to their small spatial scale. Initial studies show that these structures have been observed with increased electron temperature and electrostatic wave activity. Indicators that point to magnetic holes being a possible dissipation mechanism in turbulence. More questions need to be answered to validate whether this is the case. How do magnetic holes form? How do they evolve over time? Are there any unexpected differences between magnetic holes from different regions of Earth's magnetosphere? To answer these questions, it is important to have a large data set to work from, and that is what this project aims to achieve. By utilizing MMS, these sub-proton scale magnetic holes can be found throughout different regions of Earth's magnetosphere and cataloged with both information on the environment they were found in and of the actual magnetic hole. With this set of data, we will be able to examine the differences between magnetic holes found in the magnetosheath, magnetotail, and the foreshock and try to answer some of the questions that remain about these mysterious magnetic holes.