Speaker
Description
The ambient solar corona and solar wind plays an essential role in space weather at Earth and throughout the solar system. The magnetic field is a key aspect of describing the solar wind ambient state, and solar wind properties are closely tied to magnetic structure. The field is most readily measured in the photosphere, so models must extrapolate this field out into the solar wind. We describe a continuously updated, time-evolving MHD model of the solar corona and inner heliosphere, extending from the upper chromosphere to 1 AU, run for a month of evolution during the time leading up to the April 8, 2024 total solar eclipse. The model assimilates HMI magnetograms into a surface flux transport (SFT) model, which is used to create full-Sun boundary conditions for the MHD model. The time-evolving model is highly dynamic, with many small-scale eruptions. We compare the model results with snapshots from potential field and steady-state MHD calculations using the same boundary conditions, including differences in the magnetic connectivity predicted by the models at L1 and other spacecraft locations.
Research Supported by NASA and NSF.
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