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Hot explosions in the cool solar atmosphere

Hot explosions in the cool solar atmosphere. Hardi Peter Max Planck Institute for Solar System Research Göttingen H . Tian, W. Curdt , D . Schmit , D . Innes , B . De Pontieu , & IRIS team. Emerging AR (24. Sep. 2013) : IRIS & SDO. Si IV spectroheliogram. AIA 171 Å.

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Hot explosions in the cool solar atmosphere

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  1. Hot explosionsin the cool solar atmosphere Hardi Peter Max PlanckInstitute for Solar System Research Göttingen H. Tian, W. Curdt, D. Schmit, D. Innes, B. De Pontieu, & IRIS team

  2. Emerging AR (24. Sep. 2013): IRIS & SDO Si IV spectroheliogram AIA 171 Å these events happen at places of flux cancellation IRIS 1400 Å AIA 304 Å three bright features with lifetimes of > 5 min HMI Blos AIA 1600 Å 70” x 35”

  3. Normal spectrum: average plage

  4. Strange spectra: in abomb absorption lines ! ~5 km/s blueshift optically thin missing O IV lines same profile envelope in Mg II, C II, Si IV !! bi-directional flow

  5. Density diagnostics O IV 1400 O IV 1401 traditional density diagnostics: ratio of forbidden lines with IRIS: O IV lines around 1400 Å ≈ 0.26 → ne ≈ 4 x 1010 cm-3 O IV 1401.16 from Chianti Si IV 1403.77 O IV 1399.77 spectral radiance [DN / pixel] Doppler shift relative to target line rest wavelength [km/s] O IV 1400 O IV 1401

  6. Density diagnostics in bombs: lower limit no O IV lines upper limit: Si IV 1394 O IV 1401 Si IV 1394 O IV 1401 ≈ 10 > 700 Si IV 1403.77 O IV 1401.16 O IV 1401.16 Si IV 1403.77 O IV 1399.77 spectral radiance [DN / pixel] Doppler shift relative to target line rest wavelength [km/s]

  7. Density diagnostics in bombs: lower limit no O IV lines upper limit: Si IV 1394 O IV 1401 > 700 Si IV 1403.77 O IV 1401.16 spectral radiance [DN / pixel] → density@ Si IV origin:>5 x 1013cm-3 @ Mg II origin: >3 x 1014cm-3 → comparable to density at Tmimimum Doppler shift relative to target line rest wavelength [km/s]

  8. Summary of observations ► absorption lines (!) in EUV these line of neutral or singly ionized species have blueshifts of ~5 km/s → cool layer above energy deposition event ► still optically thin in Si IV ► bi-modal profile of Si IV (and C II, Mg II) → strong bi-directional flow (supersonic, ~ Alfven-speed) ► similar envelope of line profile in Mg II, C II, Si IV → multi-thermal flow hosting plasma over a wide Trange ► flux cancellation below brightenings → reconnection (consistent with flow speeds…) ► no O IV forbidden line emission → with other evidence: source region in high-density plasma (probably not effect of non-Maxwellian e– distribution; Dudík et al. 2014, ApJ 780, L12) ► weak ( / no) signature in 171 and 304 bands → overlying cool layer absorbs in He I and He II Lyman continua

  9. Scenario for the bombs similar to EB scenario 1 in Georgoulis et al (2002) ApJ 575, 506

  10. Relation to Ellerman bombs ? ► unclear from observations, so far… – no H-aEllerman bombs found at locations of these strange Si IV profiles (ongoing work, Vissers, G., Rouppe van der Voort et al, poster 4.21) ► some of the Si IV bombs show also coronal counterpart ► peaks of EB spectral profiles in H-a at different Doppler shifts → than Si IV and Mg II in Si IV bombs ► so far no enhancement in TR emission reported for EBs ► energy estimations: Ellerman bombs: ~1028ergs (Georgouliset al. 2002; ApJ 575, 506) Si IV bombs: ~ 1029ergs~10 x EB Si IV Si IV bomb EB QS Yang et al. (2013) Sol. Phys. 288, 39 Ellerman bomb H-a

  11. Conclusions ► highlights importance of high spectral resolution (otherwise the absorption lines would not be visible) ► energy release deep in the atmosphere (near/below T minimum) ► overlying chromosphere is pushed upwards ► huge amount of energy required to power flows and heat plasma ► how is the chromospheric plasma heated to 100.000 K or even more?► 3D MHD models predict only modest T increase…(e.g. Archontis & Hood, 2009; A&A 508, 1469) Hot explosionsin the cool solar atmosphere

  12. thanks…

  13. Line list

  14. O IV lines and kappa-distributions Dudík et al (2014, ApJ 780, L12)

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