Impact of nonthermal tails and nonthermal distributions on solar flare plasma diagnostics

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Talk presented by Jaroslav Dudík et al. at the symposium From Atoms to Stars:the impact of Spectroscopy on Astrophysics, 26th-28th July 2011, Oxford, UK

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Impact of nonthermal tails and nonthermal distributions on solar flare plasma diagnostics

  1. 1. Impact of nonthermal tails and nonthermal distributions on flare plasma diagnosticsJaroslav Dudík 1,2, Elena Dzifčáková 2, Michal Homola 1, Marian Karlický 2, Alena Kulinová 1,2, Jana Kašparová 2 1 – DAPEM, Faculty of Mathematics, Physics and Informatics, Comenius University, Bratislava, Slovakia 2 - Astronomical Institute of the Academy of Sciences Ondřejov, Czech Republic „From Atoms to Stars: The Impact of Spectroscopy on Astrophysics“, Celebrating the Career of Prof. Carole Jordan, Oxford, UK, July 27, 2011
  2. 2. OutlineI. The power-law distributions (nonthermal tails) Motivation: RHESSI flare observationsII. The n-distributions Definition and properties Seely et al. (1987) Diagnostics from observations Dzifčáková et al. (2008) Kulinová et al. (2011) Physical background Karlický et al. (2011), in prep. The nonthermal continuum Dudík et al. (2011), in prep.III. The composed np-distributions Dzifčáková et al. (2011) Construction: „know how“ Effect on ionization equilibrium and line intensities Flare plasma diagnostics
  3. 3. I. The nonthermal tailsVeronig et al. (2010), ApJ 719, 655
  4. 4. The nonthermal tailsGabriel & Phillips (1979),MNRAS 189, 319: Effect on the Fe XXIVd / Fe XXV satellite/allowed line ratios - excess excitation of the Fe XXV line - decrease of the ratio by up to 40% However, an increase is observed (even with respect to Maxwellian): Seely, Feldman & Doschek (1987), ApJ, 319, 541
  5. 5. II. The n-distributions n1 2ε1/2  ε  2 fn (ε)dε  Bn 3/2   eε/kBT dε   kBT   kBT  Peak narrower than Maxwellian Very few low-energy electrons Pseudo-temperature t : 3 n  E  kt    1  kT 2 2  Seely, Feldman & Doschek (1987), ApJ 319, 541 Dzifčáková (1998), SoPh 187, 317
  6. 6. The n-distributionsChanges in ionization and excitation equilibrium – line intensitiesContribution functions - narrower and shifted to different tDzifčáková & Tóthová (2007), SoPh 240, 211; Dudík et al. (2011), AA 529, A103
  7. 7. Diagnostics from observationsDzifčáková et al. (2008), AA 488, 311Kulinová et al. (2011), AA, accepted
  8. 8. Observed spectra - RESIK
  9. 9. Diagnostics - results
  10. 10. Theoretical f-b continuum Dudík et al. (2011), in prep.
  11. 11. Physical background - driftsKarlický, Dzifčáková & Dudík (2011), in prep.:„Moving Maxwell“ (Maxwellian with a drift velocity v0)can be written asWith the f(E,v0) having the same gradient as the n-distribution.
  12. 12. Physical background - drifts
  13. 13. Diagnostics - RHESSI Kulinová et al. (2011), AA, accepted
  14. 14. Diagnostics - RHESSI
  15. 15. III. The composed np-distributionsDzifčáková, Homola & Dudík (2011), AA 531, A111:Composed np-distribution: Bulk (n) + Tail (p)n – index n describing the bulkp – power-law index of the high-energy tailEC – low-energy cutoff for the power-law taila/b – bulk/tail ratio, a + b = 1
  16. 16. Construction of the distributionConditions for EC :- the power-law tail does not affect the plasma bulk- less than 10% discontinuity at EC
  17. 17. Construction of the distribution
  18. 18. Ionization equilibrium – tail only
  19. 19. Ionization equilibrium – bulk + tail
  20. 20. Si XIId, XIII, XIV flare spectra
  21. 21. Conclusions High-energy tail can change the ionization equilibrium Changes the temperature diagnostics from ratios of allowed lines Nonthermal bulk necessary to explain the Si XIId / Si XIII ratios - has a physical explanation – drift velocities (return current) - can also be diagnosed from RHESSI at < 6 keV Composed distributions offer simple parametrization of the true electron energy distributions in flares Easy calculation of spectra using modified CHIANTI
  22. 22. Thank you for your attention

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