Variability in Footpoint Mapping of BBFs Using Tsyganenko Models: Impact on Swarm Conjunctions

TL;DR

This study evaluates how different Tsyganenko magnetic field models affect the footpoint mapping of BBFs, revealing variability that influences magnetospheric-ionospheric studies and satellite conjunction analyses.

Contribution

It systematically analyzes the impact of input parameters on footpoint locations across multiple Tsyganenko models using a large BBF dataset.

Findings

Approximately 90% of footpoints are near midnight MLAT and MLT.

Model differences cause about +/-4° in MLAT and +/-1 hour in MLT.

Uncertainty in footpoints affects satellite conjunction counts.

Abstract

Magnetospheric-ionospheric coupling studies often rely on multi-spacecraft conjunctions, which require accurate magnetic field mapping tools. For example, linking measurements from the magnetotail with those in the ionosphere involves determining when the orbital magnetic footpoint of THEMIS or MMS intersects with the footpoint of Swarm. The Tsyganenko models are commonly used for tracing magnetic field lines. In this study, we aim to analyze how the footpoint locations are impacted by the input parameters of these models, including solar wind conditions, geomagnetic activity, and the location in the magnetotail. A dataset of 2394 bursty bulk flows (BBFs) detected by MMS was mapped to Earth's ionosphere with six different Tsyganenko models. Approximately 90% of the ionospheric footpoints are concentrated within 70{\deg} +/-5{\deg} magnetic latitude (MLAT) and +/-3 hours of magnetic local time (MLT) around midnight, with a pronounced peak in the pre-midnight sector. The MLT position showed a difference of approximately +/-1 hour MLT across the models. Footpoint locations were linked to the dawn-dusk position of the BBFs, with differences between models associated with variations in the interplanetary magnetic field clock angle. The MLAT values exhibited similar differences of approximately +/-4{\deg} around the mean value, with a systematic shift toward lower latitudes in the T89 model. This position is also influenced by the input parameters of the model representing the dynamics of Earth's magnetosphere, where stronger magnetospheric activity typically corresponds to lower latitudes. The uncertainty on the BBF footpoint location impacts the number of conjunctions with Swarm. Generally, Swarm B exhibited more conjunctions than Swarm A or C in the Northern Hemisphere.