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SUMMARY:Revised View of Solar X-Ray Jets - Dr. Alphonse Sterling (Universi
 ty of Alabama)
DTSTART:20150526T120000Z
DTEND:20150526T130000Z
UID:TALK58680@talks.cam.ac.uk
CONTACT:Andrew Hillier
DESCRIPTION:We investigate the onset of ~20 random X-ray jets observed by 
 Hinode/XRT. Each jet was near the limb in a \npolar coronal hole\, and sho
 wed a ``bright point'' in an edge of the base of the jet\, as is typical f
 or previously-observed X-ray jets. We examined SDO/AIA EUV images of each 
 of the jets over multiple AIA channels\, including 304 Å\, which detects 
 chromospheric emissions\, and 171\, 193\, and 211 Å\, which detect cooler
 -coronal emissions. We find the jets to result from eruptions of miniature
  (size <~10 arcsec) filaments from the bases of the jets. Much of the erup
 ting-filament material forms a chromospheric-temperature jet. In the cool-
 coronal channels\, often the filament appears in absorption and the hotter
  EUV component of the jet appears in emission. The jet bright point forms 
 at the location from which the miniature filament erupts\, analogous to th
 e formation of a standard solar flare arcade via flare (``internal'') reco
 nnection in the wake of the eruption of a typical larger-scale chromospher
 ic filament. The spire of the jet forms on open field lines that presumabl
 y have undergone interchange (``external'') reconnection with the erupting
  field that envelops and carries the miniature filament.  This is consiste
 nt with what we found for the onset of an on-disk coronal jet we examined 
 in Adams et al. (2014)\, and the observations of other workers.  It is how
 ever *not* consistent with the basic version of the "emerging-flux model" 
 for X-ray jets.  This work was supported by funding from NASA/LWS\, Hinode
 \, and ISSI.
LOCATION:MR14\,  Centre for Mathematical Sciences\, Wilberforce Road\, Cam
 bridge
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