A fast and slow chromospheric A fast and slow chromospheric response of H-alpha and H-beta response of H-alpha and H-beta lines to effects of accelerated lines to effects of accelerated

particles in the 26th April 2003 particles in the 26th April 2003 solar flaresolar flare

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

KotrKotrčč P. (Astronomical Institute, OndP. (Astronomical Institute, Ondřřejov), ejov),

Frolova A.S. (Irkutsk State University),Frolova A.S. (Irkutsk State University),Meshalkina N.S. (Institute of Solar-Terrestrial Physics, Meshalkina N.S. (Institute of Solar-Terrestrial Physics,

Irkutsk) Irkutsk)

Solar flare modelSolar flare model

E. Kontar, ESPM-12, E. Kontar, ESPM-12, 20082008

BackgroundBackgroundTrottet et al A&A, Trottet et al A&A,

20002000

Guangli & Haisheng // Astrophysics and Guangli & Haisheng // Astrophysics and Space Science, 2007Space Science, 2007

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

26th April 2003 solar flare 26th April 2003 solar flare

NOAA - 0338 NOAA - 0338 Flare duration 08:01– 08:09 Flare duration 08:01– 08:09 UTUT

GOES - M7.0 GOES - M7.0 Maximum– 08:07 UT Maximum– 08:07 UT

ObservationsObservations

Ondřejov Multichannel Flare Spectrograph Ondřejov Multichannel Flare Spectrograph (MFS) - chromospheric data (H(MFS) - chromospheric data (Hα and Hβ α and Hβ lines)lines)

RHESSI data (HXR)RHESSI data (HXR)Radio Solar Telescope Network database Radio Solar Telescope Network database

(RSTN) – microwave flux(RSTN) – microwave fluxSOHO/MDI, SOHO/ EIT(UV) SOHO/MDI, SOHO/ EIT(UV) KORONAS- SONG (?)KORONAS- SONG (?)

HXR vs. microwavesHXR vs. microwaves

HXR fluxes HXR fluxes

HXR vs . microwavesHXR vs . microwaves

ННαα and Н and Нβ intensity (center)β intensity (center)

HXR source movingHXR source moving

ННαα and Н and Нβ intensity (red wing)β intensity (red wing)

ННαα and Н and Нβ lines ( blue wing)β lines ( blue wing)

Simulations of subsecond effect of electron beam Simulations of subsecond effect of electron beam on Balmer series lineson Balmer series lines

KaKašparovášparová et al A&A, 2009 et al A&A, 2009

Subsecond pulses (SSP)Subsecond pulses (SSP)

Comparison of HXR, MW and chromospheric Comparison of HXR, MW and chromospheric emission during SSP for “integrated flare emission during SSP for “integrated flare

kernel”kernel”

Comparison of HXR, MW and chromospheric Comparison of HXR, MW and chromospheric emission during SSPemission during SSP

Preliminary conclusions: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.

Thank you for attention !Thank you for attention !

Solar flare modelSolar flare model