The Green Line Corona and Its Relation to the Photospheric Magnetic Field
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Abstract
Images of the green line corona made with the LASCO C1 coronagraph on SOHO are analyzed by applying current-free extrapolations to the observed photospheric eld. The Fe XIV j5303 emission is shown to be closely related to the underlying photospheric eld strength. By modeling the observed intensity patterns as a function of latitude and height above the solar limb, we derive an approximate scaling law of the form where is the density of the green lineemitting plasma and n foot P SB foot T0.9, n foot is the average eld strength at the footprints of the coronal loop. The observed high-latitude SB foot T enhancements in the green line corona are attributed to the poleward concentration of the large-scale photospheric eld. The strongest such enhancements occur where the high-latitude unipolar elds become reconnected to active region ux at lower latitudes ; the global emission pattern rotates quasirigidly at the rate of the dominant active region complex. The validity of the current-free approximation is assessed by comparing the topology of the observed and simulated green line structures.
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