Dynamics and connectivity of an extended arch filament system

Abstract

Aims. In this study, we analyzed a filament system, which expanded between moving magnetic features (MMFs) of a decaying sunspot and opposite flux outside of the active region from the nearby quiet-Sun network. This configuration deviated from a classical arch filament system (AFS), which typically connects two pores in an emerging flux region. Thus, we called this system an extended AFS. We contrasted classical and extended AFSs with an emphasis on the complex magnetic structure of the latter. Furthermore, we examined the physical properties of the extended AFS and described its dynamics and connectivity. Methods. The extended AFS was observed with two instruments at the Dunn Solar Telescope (DST). The Rapid Oscillations in the Solar Atmosphere (ROSA) imager provided images in three different wavelength regions, which covered the dynamics of the extended AFS at different atmospheric heights. The Interferometric Bidimensional Spectropolarimeter (IBIS) provided spectroscopic Hα data and spectropolarimetric data that was obtained in the near-infrared (NIR) Ca ii λ8542 Å line. We derived the corresponding line-of-sight (LOS) velocities and used He ii λ304 Å extreme ultraviolet (EUV) images of the Atmospheric Imaging Assembly (AIA) and LOS magnetograms of the Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamics Observatory (SDO) as context data.Results. The NIR Ca ii Stokes-V maps are not suitable to definitively define a clear polarity inversion line and to classify this chromospheric structure. Nevertheless, this unusual AFS connects the MMFs of a decaying sunspot with the network field. At the southern footpoint, we measured that the flux decreases over time. We find strong downflow velocities at the footpoints of the extended AFS, which increase in a time period of 30 minutes. The velocities are asymmetric at both footpoints with higher velocities at the southern footpoint. An EUV brigthening appears in one of the arch filaments, which migrates from the northern footpoint toward the southern one. This activation likely influences the increasing redshift at the southern footpoint. Conclusions. The extended AFS exhibits a similar morphology as classical AFSs, for example, threaded filaments of comparable length and width. Major differences concern the connection from MMFs around the sunspot with the flux of the neighboring quiet-Sun network, converging footpoint motions, and longer lifetimes of individual arch filaments of about one hour, while the extended AFS is still very dynamic.

Tracking Downflows from the Chromosphere to the Photosphere in a Solar Arch Filament System

“…From a theoretical point of view, Parker (1955) and Zwaan (1987) proposed that EFRs are formed in the convection zone and then emerge because of magnetic buoyancy (Parker instability) to the solar surface. During the formation process of EFRs, merging and et al 2018;Diercke et al 2019). AFSs can be observed in the He I 10830 Å triplet (e.g., Solanki et al 2003;Spadaro et al 2004;Lagg et al 2007;Xu et al 2010;González Manrique et al 2018).…”

“…The AFSs are commonly observed in several spectral lines such as in the strong chromospheric absorption line Hα, or the line core of the Ca II H & K lines (e.g., Bruzek 1969;Su et al 2018;Diercke et al 2019). AFSs can be observed in the He I 10830 Å triplet (e.g., Solanki et al 2003;Spadaro et al 2004;Lagg et al 2007;Xu et al 2010;González Manrique et al 2018).…”