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Kashapova L.K. (Institute of Solar-Terrestrial Physics, Irkutsk),

Kashapova L.K. (Institute of Solar-Terrestrial Physics, Irkutsk), Kotr č P. (Astronomical Institute, Ond ř ejov), Frolova A.S. (Irkutsk State University), Meshalkina N.S. (Institute of Solar-Terrestrial Physics, Irkutsk) ‏.

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Kashapova L.K. (Institute of Solar-Terrestrial Physics, Irkutsk),

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  1. Kashapova L.K. (Institute of Solar-Terrestrial Physics, Irkutsk), KotrčP. (Astronomical Institute, Ondřejov), Frolova A.S. (Irkutsk State University),Meshalkina N.S. (Institute of Solar-Terrestrial Physics, Irkutsk) ‏ A fast and slow chromospheric response of H-alpha and H-beta lines to effects of accelerated particles in the 26th April 2003 solar flare

  2. Solar flare model E. Kontar, ESPM-12, 2008

  3. Background Trottet et al A&A, 2000 Guangli & Haisheng // Astrophysics and Space Science, 2007 Radziszewski, Rudawy, and Phillips// A&A, 2007

  4. 26th April 2003 solar flare NOAA - 0338 Flare duration 08:01– 08:09 UT GOES - M7.0 Maximum– 08:07 UT

  5. Observations • Ondřejov Multichannel Flare Spectrograph (MFS) - chromospheric data (Hα and Hβ lines)‏ • RHESSI data (HXR)‏ • Radio Solar Telescope Network database (RSTN) – microwave flux • SOHO/MDI, SOHO/ EIT(UV) • KORONAS- SONG (?)‏

  6. HXR vs. microwaves

  7. HXR fluxes

  8. HXR vs . microwaves

  9. Нα and Нβ intensity (center)‏

  10. HXR source moving

  11. Нα and Нβ intensity (red wing)‏

  12. Нα and Нβ lines ( blue wing)‏

  13. Simulations of subsecond effect of electron beam on Balmer series lines Kašparová et al A&A, 2009

  14. Subsecond pulses (SSP)‏

  15. Comparison of HXR, MW and chromospheric emission during SSP for “integrated flare kernel”

  16. Comparison of HXR, MW and chromospheric emission during SSP

  17. Preliminary conclusions: The presence of fast and slow variations of Ha line intensity during the flare is confirmed. The same variations are found for Hβ line intensity. The Hβ line response to accelerated electrons is more informative then Ha intensity. Analysis of the obtained temporal relations allowed to reveal correlation between microwave and HXR peaks and confirmed existence of sufficient chromospheric response for subsecond times that were theoretically predicted.

  18. Thank you for attention !

  19. Solar flare model

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