Chromospheric Flashes in a Solar Pore: Insights from Multi-line Spectropolarimetric Diagnostics
Abstract
Solar pores are strongly magnetized regions lacking a photospheric penumbra and characterized by predominantly vertical magnetic fields. We present a multi-line study of flashes in a solar pore using high-resolution observations from the Swedish 1-m Solar Telescope in Fe~i~6302~, Ca~ii~8542~\ and K, and H-β, complemented by (E)UV data from IRIS and SDO/AIA. Bisector analysis and spectral inversions with SIR and NICOLE were used to infer stratifications of temperature, line-of-sight velocity, and magnetic field. Flashes, confined to one half of the pore, exhibit cooler photospheric temperatures ( T ≈ 400~K), stronger magnetic fields ( B ≈ 250~G), larger inclinations (25 versus 18), and persistent upflows (0.5~km~s-1) compared to the quiescent pore. They are co-spatial with enhanced 3- and 5-minute power in the photosphere, while only 3-minute power persists in the chromosphere. Flashes are detected down to 50\% line depth in Ca~ii~8542~\ intensity and show central chromospheric upflows (1~km~s-1) flanked by strong downflows (8~km~s-1). Temperature enhancements reach 500~K at τ ≈ -5 and 2500~K at τ ≈ -6, with a bimodal velocity distribution. Flashes correspond one-to-one with radially outward running waves near the pore boundary (5--15~km~s-1). Strong Ca~ii core emission, occasional Stokes~V reversals, and H-β enhancements indicate that pore flashes are confined to the lower and mid-chromosphere, with little influence on higher atmospheric layers.
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