Matthias Rempel | High Altitude Observatory

Chromospheric Magnetic Field Extrapolations Reveal the Flux-rope Configuration of a Solar Filament

The reconstructed three-dimensional magnetic field supporting a solar filament (top) and the corresponding filament observed by the Swedish Solar Telescope (bottom).

Data-inspired simulation of AR 11158

Top row: Photospheric (tau=0.1) magnetic field: B_z, B_x, B_y. Second row: Synthetic AIA emission in the 304, 171, and 94 passbands for a top view. Third and fourth rows: AIA emission for view along y-axis and x-axis, respectively. We show a snapshot at t=14.269 hours, which shows the ejection of a CME following an X-flare.

Near-Ultraviolet Spectropolarimetry as a tracer of Magnetic Markers of Flux Rope Formation

CMEx results

Spectropolarimetric Inversion in Four Dimensions with Deep Learning (SPIn4D): II. A Physics-Informed Machine Learning Method for 3D Solar Photosphere Reconstruction

Machine Learning Flowchart

Using the Hanle Effect in Mg II k to Quantify the Open Flux above the Solar Poles

Inversion of an average synthetic Mg II k spectrum

The Striated Solar Photosphere Observed at 0.″03 Resolution

DKIST-MURaM observations

The role of the Lorentz force in sunspot equilibrium

Scatter plot image

International & European news agencies feature Sunspot research

Sunspot Image by KIS

Cutting-edge SPIn4D project combines AI and Astronomy

SPin4D model workflow

Magnetic Field Evolution of the Solar Active Region 13664

Magnetic field configuration and parameters

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