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

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

2007-11-20

arxiv.org/abs/0711.3112v1

Astronomy and Astrophysics

Astrophysics

9 pages, 10 figures, accepted in A&A

Scientific paper

10.1051/0004-6361:20077973

We study the influence of large-scale photospheric motions on the estabilization of an eruptive filament, observed on October 6, 7, and 8, 2004, as part of an international observing campaign (JOP 178). Large-scale horizontal flows were invetigated 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. 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. We conclude that there is probably a link between changes in surface flow and the disappearance of the eruptive filament.

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