Flows in sunspot plumes detected with the Solar and Heliospheric Observatory

Bright extreme-UV sunspot plumes have been observed in eight out of 11 diff erent sunspot regions with the Coronal Diagnostic Spectrometer on Solar and Heliospheric Observatory. From wavelength shifts, we derive the line-of-si ght velocity relative to the average velocity in the rastered area, 120 " x 120 ". In sunspot plumes, we find that the motion is directed away from th e observer and increases with increasing line formation temperature, reache s a maximum between 15 and 41 km s(-1) close to log log T approximate to 5. 5, then decreases abruptly. The flow field in the corona is not well correl ated with the flow in the transition region, and we discuss briefly the imp lication of this finding.