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SUMMARY:Temperature and Density Structure of a Recurring Active Region Jet
  - Sargam Mulay (DAMTP)
DTSTART:20161011T120000Z
DTEND:20161011T130000Z
UID:TALK68130@talks.cam.ac.uk
CONTACT:Robert Teed
DESCRIPTION:We present a study of a recurring jet observed on October 31\,
  2011 by SDO/AIA\, Hinode/XRT and Hinode/EIS. We discuss the physical para
 meters of the jet such as density\, differential emission measure\, peak t
 emperature\, velocity and filling factor obtained using imaging and spectr
 oscopic observations. A differential emission measure (DEM) analysis was p
 erformed at the region of the jet-spire and the footpoint using EIS observ
 ations and also by combining AIA and XRT observations. The resulting EIS D
 EM curves were compared to those obtained with AIA-XRT. The DEM curves wer
 e used to create synthetic spectra with the CHIANTI atomic database. The p
 redicted total count rates for each AIA channel were compared with the obs
 erved count rates. The effects of varying elemental abundances and the tem
 perature range for the DEM inversion were investigated. Spectroscopic diag
 nostics were used to obtain an electron number density distribution for th
 e jet-spire and the jet-footpoint. The plasma along the line-of-sight in t
 he jet-spire and jet-footpoint was found to be peak at 2.0 MK (log T [K] =
  6.3). We calculated electron densities using the Fe XII (λ186/λ195) lin
 e ratio in the region of the spire (Ne = 7.6×10^10 cm^−3 ) and the foot
 point (1.1×10^11 cm^−3 ). The plane-of-sky velocity of the jet is found
  to be 524 km/s. The resulting EIS DEM values are in good agreement with t
 hose obtained from AIA-XRT. The synthetic spectra contributing to each AIA
  channel confirms the multi-thermal nature of the AIA channels in both reg
 ions. There is no indication of high temperatures\, such as emission from 
 Fe XVII (λ254.87) (log T [K] = 6.75) seen in the jet-spire. In case of th
 e jet-footpoint\, synthetic spectra predict weak contributions from Ca XVI
 I (λ192.85) and Fe XVII (λ254.87). With further investigation\, we confi
 rmed emission from the Fe XVIII (93.932 Å) line in the AIA 94 Å channel 
 in the region of the footpoint. We also found good agreement between the e
 stimated and predicted Fe XVIII count rates. A study of the temporal evolu
 tion of the jet-footpoint and the presence of high-temperature emission fr
 om the Fe XVIII (λ93.932) (log T [K] = 6.85) line leads us to conclude th
 at the hot component in the jet-footpoint was present initially that the j
 et had cooled down by the time EIS observed it.
LOCATION:MR11\,  Centre for Mathematical Sciences\, Wilberforce Road\, Cam
 bridge
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