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Emerging Flux and the Heating of Coronal Loops

Published online by Cambridge University Press:  26 May 2016

B. Schmieder ,
P. Démoulin ,
D.M. Rust ,
M.K. Georgoulis  and
P.N. Bernasconi
B. Schmieder
Affiliation:
1Observatoire de Paris, LESIA, 92195 Meudon Cedex, France 2ITA, University of Oslo, Blindern, N-0315, Oslo, Norway
P. Démoulin
Affiliation:
1Observatoire de Paris, LESIA, 92195 Meudon Cedex, France
D.M. Rust
Affiliation:
3JHU/APL, 11100 John Hopkins Road, Laurel MD 20723-6099, USA
M.K. Georgoulis
Affiliation:
3JHU/APL, 11100 John Hopkins Road, Laurel MD 20723-6099, USA
P.N. Bernasconi
Affiliation:
3JHU/APL, 11100 John Hopkins Road, Laurel MD 20723-6099, USA

Abstract

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Observations of various instruments on board Yohkoh, SOHO, and TRACE complement high-resolution observations of the balloon-borne Flare Genesis Experiment, obtained on January 25, 2000. A subset of the TRACE loops are located in the vicinity of the SXT loops in the NOAA emerging active region 8844, but never coincide with them. We find that coronal loops appeared 6 ± 2 hr after the first detection of emerging magnetic flux. The loops evolved rapidly when the active region entered its impulsive flux emergence phase. In the low chromosphere, flux emergence was reflected in intense Ellerman bomb activity. Besides chromosphere, we find that Ellerman bombs may also heat the transition region, by contributing to the moss emission. Areas prolific in Ellerman bombs show moss ∼ 100% brighter than areas without Ellerman bombs. Only the strongest Ellerman bombs can heat their surroundings to coronal temperatures. In the corona, we find a spatio-temporal anti-correlation between the soft X-ray (SXT) and the extreme ultraviolet (TRACE) loops: First, the SXT loops preceded the appearance of the TRACE loops by 30 — 40 min. Second, the TRACE loops had different shapes and different footpoints compared to the SXT loops. The SXT and TRACE loops are probably formed independently.

Type
Part 9: Heating of Solar and Stellar Coronae
Information
Symposium - International Astronomical Union , Volume 219: Stars as Suns : Activity, Evolution and Planets , 2004 , pp. 483 - 487
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

Bernasconi, P. N., Rust, D., M., Georgoulis, M. K., & Labonte, B. J. 2002, Solar Phys, 209, 119.CrossRefGoogle Scholar
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Schmieder, B., Georgoulis, M. K., Rust, D. M., Démoulin, P., & Bernasconi, P. N. 2004, ApJ, in press.Google Scholar