Abstract Quiescent filaments are prominent features of the solar atmosphere, and their evolution reflects the coronal magnetic field’s response to photospheric magnetic activity. Here, we report on a quiescent filament observed on 2023 September 28–29, aiming to understand how the magnetic configuration shapes its feet and drives its extension. For this purpose, high-resolution spectral data in H α and Mg II k are used from the Télescope Héliographique pour l’Etude du Magnétisme et des Instabilités Solaires and the Interface Region Imaging Spectrograph, respectively. To track changes in the filament, we utilise long-term data from the Atmospheric Imaging Assembly on the Solar Dynamics Observatory (SDO) and from the Global Oscillation Network Group (GONG). We analyse the longitudinal magnetic field in the photosphere using the Solar Optical Telescope on board Hinode, as well as SDO/Helioseismic and Magnetic Imager data. In addition to this, we use GONG H α data to analyze the longitudinal oscillations in the filament. Observations show that parasitic polarities and canceling flux play a key role in forming and reorganizing the filament feet and in lengthening the filament. A 3D MHD reconstruction using vector magnetograms reveals that its magnetic configuration evolves into a full flux rope (FR), whose extension on the second day matches the observed filament growth. The FR is separated from the surrounding nearly potential field by quasi-separatrix layers, which in turn are separated by current layers. They get more organized around the FR as it grows. Moreover, the longitudinal oscillations in the extended filament are attributed to heating from flux cancellation at underlying bright points.
Karki et al. (Fri,) studied this question.