Astron. Astrophys. 324, 324-328 (1997)

The chromospheric response due to filament eruption

B.P. Filippov

Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation, Russian Academy of Sciences, 142092, Troitsk Moscow Region, Russia

Received 4 October 1996 / Accepted 12 December 1996

Abstract

Frozen-in motion of chromospheric plasma during an eruption of a filament of inverse polarity is considered. At the initial stage of the filament ascent, magnetic field compresses the chromospheric plasma within two belts disposed bilaterally along a polarity inversion line. Compression should be accompanied by heating of plasma and enhancement of emission in H . The distance between the belts increases as the filament ascends. The estimates show that this mechanism can be effective to represent the H flare kernels dynamics in two-ribbon flares.

Key words: Sun: chromosphere Sun: filaments Sun: magnetic fields

Send offprint requests to: B.P. Filippov

Contents

• 1. Introduction
• 2. Magnetic field of a model
• 3. Frozen-in chromospheric plasma motion
• 4. Compression and heating of the chromosphere
• 5. Energy estimates
• 6. Conclusions
• Acknowledgements
• References

© European Southern Observatory (ESO) 1997

Online publication: May 26, 1998

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