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Title: OSCILLATING LIGHT WALL ABOVE A SUNSPOT LIGHT BRIDGE

Abstract

With the high tempo-spatial Interface Region Imaging Spectrograph 1330 Å images, we find that many bright structures are rooted in the light bridge of NOAA 12192, forming a light wall. The light wall is brighter than the surrounding areas, and the wall top is much brighter than the wall body. The New Vacuum Solar Telescope Hα and the Solar Dynamics Observatory 171 and 131 Å images are also used to study the light-wall properties. In 1330, 171, and 131 Å, the top of the wall has a higher emission, while in the Hα line, the wall-top emission is very low. The wall body corresponds to bright areas in 1330 Å and dark areas in the other lines. The top of the light wall moves upward and downward successively, performing oscillations in height. The deprojected mean height, amplitude, oscillation velocity, and the dominant period are determined to be 3.6 Mm, 0.9 Mm, 15.4 km s{sup −1}, and 3.9 minutes, respectively. We interpret the oscillations of the light wall as the leakage of p-modes from below the photosphere. The constant brightness enhancement of the wall top implies the existence of some kind of atmospheric heating, e.g., via the persistent small-scale reconnection ormore » the magneto-acoustic waves. In another series of 1330 Å images, we find that the wall top in the upward motion phase is significantly brighter than in the downward phase. This kind of oscillation may be powered by the energy released due to intermittent impulsive magnetic reconnection.« less

Authors:
; ;  [1];  [2]
  1. Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012 (China)
  2. Fuxian Solar Observatory, Yunnan Observatories, Chinese Academy of Sciences, Kunming 650011 (China)
Publication Date:
OSTI Identifier:
22518983
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal Letters
Additional Journal Information:
Journal Volume: 804; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 2041-8205
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; BRIGHTNESS; HEATING; IMAGES; MAGNETIC RECONNECTION; OSCILLATIONS; PHOTOSPHERE; SOUND WAVES; SUN; SUNSPOTS; TELESCOPES; ULTRAVIOLET RADIATION; VISIBLE RADIATION

Citation Formats

Yang, Shuhong, Zhang, Jun, Jiang, Fayu, and Xiang, Yongyuan, E-mail: shuhongyang@nao.cas.cn. OSCILLATING LIGHT WALL ABOVE A SUNSPOT LIGHT BRIDGE. United States: N. p., 2015. Web. doi:10.1088/2041-8205/804/2/L27.
Yang, Shuhong, Zhang, Jun, Jiang, Fayu, & Xiang, Yongyuan, E-mail: shuhongyang@nao.cas.cn. OSCILLATING LIGHT WALL ABOVE A SUNSPOT LIGHT BRIDGE. United States. doi:10.1088/2041-8205/804/2/L27.
Yang, Shuhong, Zhang, Jun, Jiang, Fayu, and Xiang, Yongyuan, E-mail: shuhongyang@nao.cas.cn. Sun . "OSCILLATING LIGHT WALL ABOVE A SUNSPOT LIGHT BRIDGE". United States. doi:10.1088/2041-8205/804/2/L27.
@article{osti_22518983,
title = {OSCILLATING LIGHT WALL ABOVE A SUNSPOT LIGHT BRIDGE},
author = {Yang, Shuhong and Zhang, Jun and Jiang, Fayu and Xiang, Yongyuan, E-mail: shuhongyang@nao.cas.cn},
abstractNote = {With the high tempo-spatial Interface Region Imaging Spectrograph 1330 Å images, we find that many bright structures are rooted in the light bridge of NOAA 12192, forming a light wall. The light wall is brighter than the surrounding areas, and the wall top is much brighter than the wall body. The New Vacuum Solar Telescope Hα and the Solar Dynamics Observatory 171 and 131 Å images are also used to study the light-wall properties. In 1330, 171, and 131 Å, the top of the wall has a higher emission, while in the Hα line, the wall-top emission is very low. The wall body corresponds to bright areas in 1330 Å and dark areas in the other lines. The top of the light wall moves upward and downward successively, performing oscillations in height. The deprojected mean height, amplitude, oscillation velocity, and the dominant period are determined to be 3.6 Mm, 0.9 Mm, 15.4 km s{sup −1}, and 3.9 minutes, respectively. We interpret the oscillations of the light wall as the leakage of p-modes from below the photosphere. The constant brightness enhancement of the wall top implies the existence of some kind of atmospheric heating, e.g., via the persistent small-scale reconnection or the magneto-acoustic waves. In another series of 1330 Å images, we find that the wall top in the upward motion phase is significantly brighter than in the downward phase. This kind of oscillation may be powered by the energy released due to intermittent impulsive magnetic reconnection.},
doi = {10.1088/2041-8205/804/2/L27},
journal = {Astrophysical Journal Letters},
issn = {2041-8205},
number = 2,
volume = 804,
place = {United States},
year = {2015},
month = {5}
}