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The solar active region photospheric magnetic field evolves rapidly duringmajor eruptive events, suggesting appreciable feedback from the corona.Previous studies of these "magnetic imprints" are mostly based on line-of-sightonly or lower-cadence vector observations; a temporally resolved depiction ofthe vector field evolution is hitherto lacking. Here, we introduce thehigh-cadence (90~s or 135~s) vector magnetogram dataset from the Helioseismicand Magnetic Imager (HMI) that is well suited for investigating the phenomenon.These observations allow quantitative characterization of the permanent,step-like changes that are most pronounced in the horizontal field component($B_h$). A highly structured pattern emerges from analysis of an archetypicalevent, \texttt{SOL2011-02-15T01:56}, where $B_h$ near the main polarityinversion line increases significantly during the earlier phase of theassociated flare with a time scale of several minutes, while $B_h$ in theperiphery decreases at later times with smaller magnitudes and a slightlylonger time scale. The dataset also allows effective identification of the"magnetic transient" artifact, where enhanced flare emission alters the Stokesprofiles and the inferred magnetic field becomes unreliable. Our resultsprovide insights on the momentum processes in solar eruptions. The dataset mayalso be useful to the study of sunquakes and data-driven modeling of thecorona.

Investigating the Magnetic Imprints of Major Solar Eruptions with SDO/HMI High-Cadence Vector Magnetograms