Solar Magnetism and Atmospheric Dynamics
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SoMAD is the research theme that connects my work on waves, coronal-loop dynamics, reconnection-driven activity, and long-term solar magnetic variability. It focuses on how magnetic fields and plasma flows shape the solar atmosphere across timescales from seconds to solar cycles.
Waves and energy transport
How do waves propagate, damp, and transfer energy through magnetised solar plasma?
Transverse and longitudinal MHD waves in coronal loops, plumes, and fibrils
Observations from Solar Orbiter/EUI, SDO/AIA, IRIS, Hinode
Forward modelling and simulations to interpret damping, visibility, and energetics
Magnetic reconnection and dynamic coupling
How does magnetic energy get converted into heat, flows, and waves?
Jets, brightenings, fibrils, and reconnection-driven dynamics
Multi-wavelength diagnostics across the lower and upper atmosphere
Comparison with numerical models and magnetic-field extrapolations
Long-term solar variability
How does solar magnetism evolve from active regions to solar cycles?
Historical sunspot area catalogues from Kodaikanal and other observatories
Calibrated long-term datasets for irradiance and solar-cycle studies
Applications to active longitudes, sunspot statistics, and magnetic variability
Solar feature detection and archives
How can we extract reliable physics from large solar archives?
Automated detection of sunspots, plages, filaments, and other features
Image processing and machine-learning tools for historical and modern datasets
Public catalogues and derived data products
Application of a neural network on historical sunspot images: Loan, Mandal & Krivova
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