Observation of solar coronal heating powered by magneto-acoustic oscillations in a moss region

• Published in: Research in astronomy and astrophysics Vol. 21; no. 4; pp. 105 - 252
• Main Authors: Hashim, Parida, Hong, Zhen-Xiang, Ji, Hai-Sheng, Shen, Jin-Hua, Ji, Kai-Fan, Cao, Wen-Da
• Format: Journal Article
• Language: English
• Published: Beijing National Astronomical Observatories, CAS and IOP Publishing Ltd 01.05.2021; IOP Publishing; Graduate School of the Chinese Academy of Sciences,Beijing 100871,China; Xinjiang Astronomical Observatory,Chinese Academy of Sciences,Urumqi 830011,China%Purple Mountain Observatory,DMSA/CAS,Nanjing 210023,China%Purple Mountain Observatory,DMSA/CAS,Nanjing 210023,China; CfASS,China Three Gorges University,Yichang 443002,China%Xinjiang Astronomical Observatory,Chinese Academy of Sciences,Urumqi 830011,China%Yunnan Astronomical Observatory,Chinese Academy of Sciences,Kunming 830011,China%Big Bear Solar Observatory,40386 North Shore Lane,Big Bear City,CA 922314,USA
• Subjects: Absorption; Acoustic emission; Acoustic waves; Acoustics; Chromosphere; Corona; Coronal heating; Data analysis; Energy flow; Heating; Helium; High resolution; Image resolution; Magnetic fields; Magnetic loops; Magnetoacoustic oscillations; Mosses; Observatories; Photosphere; Solar activity; Solar corona; Solar observatories; Solar power; Solar transition region; Sun: chromosphere; Sun: corona; Sun: magnetic field; Sun:corona; Sun:chromosphere; Sun:magnetic field
• ISSN: 1674-4527; 2397-6209
• DOI: 10.1088/1674-4527/21/4/105

Abstract In this paper, we report the observed temporal correlation between extreme-ultraviolet (EUV) emission and magneto-acoustic oscillations in an EUV moss region, which is the footpoint region only connected by magnetic loops with million-degree plasma. The result is obtained from a detailed multi-wavelength data analysis of the region with the purpose of resolving fine-scale mass and energy flows that come from the photosphere, pass through the chromosphere and finally heat the solar transition region or the corona. The data set covers three atmospheric levels on the Sun, consisting of high-resolution broad-band imaging at TiO 7057 Å and the line of sight magnetograms for the photosphere, high-resolution narrow-band images at helium i 10830 Å for the chromosphere and EUV images at 171 Å for the corona. The 10830 Å narrow-band images and the TiO 7057 Å broad-band images are from a much earlier observation on 2012 July 22 with the 1.6 meter aperture Goode Solar Telescope (GST) at Big Bear Solar Observatory (BBSO) and the EUV 171 Å images and the magnetograms are from observations made by Atmospheric Imaging Assembly (AIA) or Helioseismic and Magnetic Imager (HMI) onboard the Solar Dynamics Observatory (SDO). We report the following new phenomena: (1) Repeated injections of chromospheric material appearing as 10830 Å absorption are squirted out from inter-granular lanes with a period of ∼ 5 minutes. (2) EUV emissions are found to be periodically modulated with similar periods of ∼ 5 minutes. (3) Around the injection area where 10830 Å absorption is enhanced, both EUV emissions and strength of the magnetic field are remarkably stronger. (4) The peaks on the time profile of the EUV emissions are found to be in sync with oscillatory peaks of the stronger magnetic field in the region. These findings may give a series of strong evidences supporting the scenario that coronal heating is powered by magneto-acoustic waves.