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Abstract
Bright extreme-UV sunspot plumes have been observed in eight out of 11 different sunspot regions with the Coronal Diagnostic Spectrometer on Solar and Heliospheric Observatory. From wavelength shifts, we derive the line-of-sight velocity relative to the average velocity in the rastered area, 120'' × 120''. In sunspot plumes, we find that the motion is directed away from the observer and increases with increasing line formation temperature, reaches a maximum between 15 and 41 km s-1 close to log logT ≈ 5.5, then decreases abruptly. The flow field in the corona is not well correlated with the flow in the transition region, and we discuss briefly the implication of this finding.
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