How eruptions of a small filament feed materials to a nearby larger-scaled filament. (31st August 2020)

• Record Type: Journal Article
• Authors: Wei, H; Huang, Z; Hou, Z; Qi, Y; Fu, H; Li, B; Xia, L
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 498:Number 1(2020)
• Page Start: L104
• Page End: L108
• Publication Date: 2020-08-31
• Subjects: Sun: atmosphere -- Sun: filaments -- Sun: activity -- magnetic reconnection -- Sun: chromosphere -- methods: data analysis; Astronomy -- Research -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnrasl/slaa134
• Languages: English
• ISSNs: 1745-3933

Abstract

ABSTRACT: As one of the most common features in the solar atmosphere, filaments are significant not only in solar physics but also in stellar and laboratory plasma physics. With the New Vacuum Solar Telescope and the Solar Dynamics Observatory, here we report on multi-wavelength observations of eruptions of a small (30 arcsec) filament (SF) and its consequences while interacting with ambient magnetic features including a large (300 arcsec) filament (LF). The eruptions of the SF drive a two-side-loop jet that is a result of magnetic reconnection between the SF threads and an overlying magnetic channel. As a consequence of the eruption, the heating in the footpoints of the SF destabilizes the barbs of the LF rooted nearby. Supersonic chromospheric plasma flows along the barbs of the LF are then observed in the H α passband and they apparently feed materials to the LF. We suggest that they are shock-driven plasma flows or chromospheric evaporations, which can both be the consequences of heating in the chromosphere by non-thermal particles generated in the magnetic reconnection associated with the two-side-loop jet. Our observations demonstrate that the destabilization in the vicinity of the footpoints of a barb can drive chromospheric plasma feeding to the filament.