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Two TR papers from the ITA...

Two TR papers from the ITA. Guerreiro et al 2013, «Cycling of material between the solar corona and chromospheere», on 2nd revision in ApJ Olluri et al 2013, «Non equilibrium ionization effects on the density line ratio diagnostics of O IV», on 2nd revision in ApJ.

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Two TR papers from the ITA...

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  1. Two TR papers from the ITA... • Guerreiro et al 2013, «Cycling of material between the solar corona and chromospheere», on 2nd revision in ApJ • Olluri et al 2013, «Non equilibrium ionization effects on the density line ratio diagnostics of O IV», on 2nd revision in ApJ

  2. How do the TR and corona maintain a more or less constant mass when material is cycling very rapidly?

  3. Tracer fluid inserted in TR for ranges [20,300]kK and [300,700] kK and followed for two minutes • TR emptied of material very rapidly - only 10% remains after 2 minutes - both to hotter and cooler domains • Not steady state flow up or down temperature gradient

  4. Most TR material collects in upper chromosphere... • ...but significant fraction is heated and attains high velocites

  5. left panel: Most TR loops are low (< 4 Mm) and low loops have the most TR (e.g. C IV 1548 Å) emissivity • right panel: A majority of TR loops have low Tgmax, but a significant fraction reaches coronal temperatures • red-shift mainly due vigorously heated low lying loops - heating expels material, cooling re-fills loop...

  6. Heating short loop Cooling short loop Low loop examples velocity is along loop length ‘s’ time (240 s) runs from black via blue/green/yellow to red

  7. Typical heated coronal loop Note heating near TR, note velocity pattern in TR time (240 s) runs from black via blue/green/yellow to red

  8. How will non-equilibrium ionization affect the IRIS O IV density sensitive line ratio?

  9. 24x24x14.5 Mm model, with «bipole» magnetic field configuration.TR is well spread in height

  10. O is far from equilibrium in a typical model TR (e.g. velocities, densities, and temperature gradients as «expected»)

  11. Emergent log(intensity) in O IV 1401 Å spectral line in statistical equilibrium (upper panel)and in non-equilibrium

  12. If O IV were in equilibrium, density sensitive line pair would be a very good diagnostic of the density at 140 kK.But it is NOT and the line pair therefore gives an overestimate of the density, up to greater than factor 5=> A significant portion of NEQ O IV is radiating at lower temperatures/higher densities than in SENo obvious connection with velocity pattern in TR

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