Frequent EUV microflashes at solar plume bases, each releasing ~10^24 erg, are identified as a new unipolar network event and suggested as a candidate mechanism to power the open corona and solar wind.
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Realistic 3D MHD modeling of observed active region AR 11166 reproduces key observed properties of quasi-periodic fast propagating magnetosonic waves with improved qualitative agreement over idealized setups.
Simulations demonstrate that fast magnetoacoustic waves incident on a localized coronal null undergo mode conversion to produce incompressible energetic Alfvén wave packets along separatrices.
Shock waves from nonlinear steepening in the chromosphere drive spicules, transition to large-amplitude compressive MHD waves in the corona depending on field strength, produce PCDs, show period evolution from ~5 to >=10 minutes, and supply mass flux toward the solar wind.
A visual transformer model trained on IRIS inversions predicts chromospheric temperature and density from SDO data with correlations around 0.8 on 80% of test cases.
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Modeling the Excitation, Propagation and Damping of Quasi-Periodic Fast Magnetosonic Waves in Realistic Coronal Active Region Magnetic Field Structures
Realistic 3D MHD modeling of observed active region AR 11166 reproduces key observed properties of quasi-periodic fast propagating magnetosonic waves with improved qualitative agreement over idealized setups.