Publication Date:
2023-07-31
Description:
Global magnetohydrodynamic (MHD) modeling of the solar corona, applicable to specific time periods, is now over 25 years old. In the standard approach, synoptic maps of the photospheric magnetic field, available from different observatories, are used to derive the boundary conditions, and the equations are integrated in time until a steady-state is reached. The models have increased in sophistication over the years, and their output can be used to simulate many observables, including EUV and X-ray emission, scattering of white-light, and ion charge-state abundances. The models can reproduce many aspects of coronal structure, but also show limitations in their ability to predict some phenomena. In this talk, we focus on two aspects that we believe will likely garner increased attention in the coming years: 1) The inclusion of finer scale details in the magnetic boundary conditions, and how it leads to structuring of the corona and solar wind; and 2) Time-dependent models of the solar corona, driven by evolving surface magnetic fields as captured by flux transport models.
Language:
English
Type:
info:eu-repo/semantics/conferenceObject
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