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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 Kashapova L.K.

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Presentation on theme: "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 Kashapova L.K."— Presentation transcript:

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

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 Radziszewski, Rudawy, and Phillips// A&A, 2007

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

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