Covert connection of filaments

Abstract

We analyse the relationship between two near filaments, which do not show any connection in H-alpha images but reveal close magnetic connectivity during filament activations in Extreme Ultraviolet (EUV) observations. A twisted flux rope, which connects a half of one filament with another filament, becomes visible during several activations but seems to exist all the time of the filaments presence on the disc. Solar Dynamic Observatory} (SDO) and Solar Terrestrial Relations Observatory (STEREO) observed the region with the filaments from two points of view separated by the angle of about 120 deg. On 2012 July 27, SDO observed the filament activation on disc, while for the STEREO B position the filaments were visible at the limb. Nearly identical interaction episode was observed on 2012 August 04 by STEREO A on disc and by SDO at the limb. This good opportunity allows us to disentangle the 3-D shape of the connecting flux rope and in particular to determine with high reliability the helicity sign of the flux rope, which looks ambiguous in preliminary inspections of on-disc EUV images only.} The complex magnetic structure of the region consists of three braided flux ropes in the vicinity of the coronal null point. Using observations of the flux rope fine structure and plasma motions within it from two points of view, we determine the negative sign of helicity of the flux rope, which corresponds to dextral chirality of the filaments. The observations, despite the tangled fine structure in some EUV images, support flux rope filament models. They give more evidence for the one-to-one relationship between the filament chirality and the flux rope helicity.

13 pages, 12 figures, to appear in MNRAS

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Cited by in corpus (2)

• Large-Amplitude Longitudinal Oscillations Triggered by the Merging of Two Solar Filaments: Observations and Magnetic Field Analysis
• Interchange reconnection associated with a confined filament eruption: Implications for the source of transient cold-dense plasma in solar winds