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EUV Doppler shifts as a Signature of Transient Heating in the Solar Corona

EUV Doppler shifts as a Signature of Transient Heating in the Solar Corona. Youra Taroyan & Keiran Burrows BUKS Meeting 5 July 2012. Pre-Hinode EUV Doppler shift measurements. Peter & Judge (1999) Teriaca et al. (1999). Hinode / EIS. Hara et al. 2008, etc.

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EUV Doppler shifts as a Signature of Transient Heating in the Solar Corona

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  1. EUV Doppler shifts as a Signature of Transient Heating in the Solar Corona Youra Taroyan & Keiran Burrows BUKS Meeting 5 July 2012

  2. Pre-Hinode EUV Doppler shift measurements Peter & Judge (1999) Teriaca et al. (1999)

  3. Hinode / EIS • Hara et al. 2008, etc. Blue-red asymmetry Double Gaussian

  4. Observations • Active region visible on 20 February 2007 • EIS scans of the active region with the 1’’ slit. • Spectral data for a number of lines produced Analysis • Three iron lines selected: Fe VIII 185, Fe X 184.5, Fe XII 195 • Standard procedures, line spectra fitted by single Gaussians • Intensity and Doppler velocity maps produced

  5. Observations

  6. Thermal conduction Heating rate Radiation 1D loop modelling using HYDRAD (Bradshaw & Mason 2003)

  7. Observer

  8. Synthesis of spectral line profiles • -Line intensity • -Emissivity of the line • -Line broadening function • Doppler width of the line • Doppler shift

  9. Spectroscopic consequences of repetitive heating

  10. Synthesized Observed

  11. Heating associated with blue shifts Cooling associated with red shifts Transition from heating to cooling or vice-versa  no shifts Two types of line profiles for Fe XII Fe viii red shifts Fe x small shifts  repetitive footpoint heating on a time scale of a few minutes Reducing heating duration (<1 min)  no association Longer (>16 min) duration or heating not localised at the footpoints  no high speed flows Conclusions Observations & simulations

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