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.
Decayless transverse waves in coronal loops: Mandal et al A&A, 652, L3 (2021)
Waves and Energy Transport
Question: 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.
Capturing smallest-scale solar jet: Mandal et al, 664, A28 (2022)
Magnetic Reconnection and Dynamic Coupling
Question: 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
Question: 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 solar magnetic variability.
Calibrating historical sunspot archives: Mandal et al A&A, 640, A78 (2020)
Solar Feature Detection and Long-term Archives
Question: 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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