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Large-scale horizontal flows in the solar photosphere. III. Effects on filament destabilization

By T. Roudier, M. Švanda, N. Meunier, S. Keil, M. Rieutord, J. M. Malherbe, S. Rondi, G. Molodij, V. Bommier and B. Schmieder


9 pages, 10 figures, accepted in A&AInternational audienceAims.We study the influence of large-scale photospheric motions on the destabilization of an eruptive filament, observed on October 6, 7, and 8, 2004, as part of an international observing campaign (JOP 178). Methods: Large-scale horizontal flows were investigated from a series of MDI full-disc Dopplergrams and magnetograms. From the Dopplergrams, we tracked supergranular flow patterns using the local correlation tracking (LCT) technique. We used both LCT and manual tracking of isolated magnetic elements to obtain horizontal velocities from magnetograms. Results: We find that the measured flow fields obtained by the different methods are well-correlated on large scales. The topology of the flow field changed significantly during the filament eruptive phase, suggesting a possible coupling between the surface flow field and the coronal magnetic field. We measured an increase in the shear below the point where the eruption starts and a decrease in shear after the eruption. We find a pattern in the large-scale horizontal flows at the solar surface that interact with differential rotation. Conclusions: We conclude that there is probably a link between changes in surface flow and the disappearance of the eruptive filament

Topics: Sun: filaments, Sun: atmosphere, Sun: magnetic fields, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph]
Publisher: 'EDP Sciences'
Year: 2008
DOI identifier: 10.1051/0004-6361:20077973
OAI identifier: oai:HAL:hal-00286952v1
Provided by: HAL-INSU
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