Heating of quiescent coronal loops caused by nearby eruptions observed with the Solar Dynamics Observatory and the Solar Upper Transition Region Imager
arXiv:2303.15758 · doi:10.3847/1538-4357/acc8c6
Abstract
How structures, e.g., magnetic loops, in the upper atmosphere, i.e., the transition region and corona, are heated and sustained is one of the major unresolved issues in solar and stellar physics. Various theoretical and observational studies on the heating of coronal loops have been undertaken. The heating of quiescent loops caused by eruptions is, however, rarely observed. In this study, employing data from the Solar Dynamics Observatory (SDO) and Solar Upper Transition Region Imager (SUTRI), we report the heating of quiescent loops associated with nearby eruptions. In active regions (ARs) 13092 and 13093, a long filament and a short filament, and their overlying loops are observed on 2022 September 4. In AR 13093, a warm channel erupted toward the northeast, whose material moved along its axis toward the northwest under the long filament, turned to the west above the long filament, and divided into two branches falling to the solar surface. Subsequently, the short filament erupted toward the southeast. Associated with these two eruptions, the quiescent loops overlying the long filament appeared in SDO/Atmospheric Imaging Assembly (AIA) high-temperature images, indicating the heating of loops. During the heating, signature of magnetic reconnection between loops is identified, including the inflowing motions of loops, and the formation of X-type structures and newly reconnected loops. The heated loops then cooled down. They appeared sequentially in AIA and SUTRI lower-temperature images. All the results suggest that the quiescent loops are heated by reconnection between loops caused by the nearby warm channel and filament eruptions.
20 pages, 12 figures, accepted for publication in ApJ
References in corpus (20)
- Coronal heating by MHD waves
- Multi-scale Gaussian normalization for solar image processing
- Persistent Doppler shift oscillations observed with HINODE/EIS in the solar corona: spectroscopic signatures of Alfvenic waves and recurring upflows
- JHelioviewer - Time-dependent 3D visualisation of solar and heliospheric data
- Global maps of the magnetic field in the solar corona
- Solar Coronal Loops Associated with Small-scale Mixed Polarity Surface Magnetic Fields
- Multiwavelength observations of a partially eruptive filament on 2011 September 8
- Round-trip Slipping Motion of the Circular Flare Ribbon Evidenced in a Fan-spine Jet
- On the Brightening Propagation of Post-Flare Loops Observed by TRACE
- Conversion from mutual helicity to self-helicity observed with IRIS
- Toward a Unified Explanation for the Three-part Structure of Solar Coronal Mass Ejections
- First detection of transverse vertical oscillation during the expansion of coronal loops
- The Structure of Solar Coronal Mass Ejections in the Extreme-Ultraviolet Passbands
- Miniature loops in the solar corona
- Formation of solar quiescent coronal loops through magnetic reconnection in an emerging active region
- Magnetic reconnection between loops accelerated by a nearby filament eruption
- Formation of a solar filament by magnetic reconnection and coronal condensation
- Failed Solar Eruption of A Multi-thermal Flux Rope
- Revisiting the formation mechanism for coronal rain from previous studies
- An investigation of flare emissions at multiple wavelengths