Fast Dimming Associated with a Coronal Jet Seen in Multi-Wavelength and Stereoscopic Observations

  • Lee, K.S. (Department of Astronomy and Space Science, Kyung Hee University) ;
  • Innes, D.E. (Max-Planck Institute for Solar System Research) ;
  • Moon, Y.J. (Department of Astronomy and Space Science, Kyung Hee University) ;
  • Shibata, K. (Kwasan and Hida Observatories, Kyoto University) ;
  • Lee, Jin-Yi (Department of Astronomy and Space Science, Kyung Hee University)
  • Published : 2012.04.03


We have investigated a coronal jet observed near the limb on 2010 June 27 by the Hinode/X-Ray Telescope (XRT), EUV Imaging Spectrograph (EIS), and Solar Optical Telescope (SOT), and the SDO/Atmospheric Imaging Assembly (AIA), Helioseismic and Magnetic Imager (HMI), and on the disk by STEREO-A/EUVI. From EUV (AIA and EIS) and soft X-ray (XRT) images we have identified both cool and hot jets. There was a small loop eruption in Ca II images of the SOT before the jet eruption. Using high temporal and multi wavelength AIA images, we found that the hot jet preceded its associated cool jet by about 2 minutes. The cool jet showed helical-like structures during the rising period. According to the spectroscopic analysis, the jet's emission changed from blue to red shift with time, implying helical motions in the jet. The STEREO observation, which enabled us to observe the jet projected against the disk, showed that there was a dim loop associated with the jet. We have measured a propagation speed of ~800 km/s for the dimming front. This is comparable to the Alfven speed in the loop computed from a magnetic field extrapolation of the HMI photospheric field measured 5 days earlier and the loop densities obtained from EIS Fe XIV line ratios. We interpret the dimming as indicating the presence of Alfvenic waves initiated by reconnection in the upper chromosphere.