Quantifying Chromosphere Response to Flare Energy Release Using AIA Observations in 1600 Å and 304 Å Passbands

IF 2.4 3区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS
Jiong Qiu, Rhiannon Fleming
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Abstract

Imaging observations of the solar lower atmosphere by the Atmospheric Imaging Assembly (AIA) have been mostly used as the context, and their quantitative information has been much less explored. The chromosphere responds rapidly to energy release by magnetic reconnection during flares. Furthermore, a flare is a collection of multiple energy release events that can be identified in spatially resolved chromosphere observations. In this paper, we conduct a statistical and semi-quantitative study of the relative photometry in the UV 1600 Å and EUV 304 Å passbands for 18 flares observed by AIA. In each flare, we have identified thousands of flare ribbon pixels in the UV 1600 Å images, and measured their brightness (counts per second) and the rise and decay timescales, which are indicative of heating properties in flare loops. The analysis shows that bright flare pixels, characterized by peak brightness larger than ten times the quiescent brightness, exhibit sharplight curves with the half rise time below 2 min, followed by a two-phase decay with a rapid decay on timescales comparable to the rise time and then a more gradual decay. Flare ribbon pixels identified in both UV 1600 Å and EUV 304 Å images exhibit similar time profiles during the rise, and their peak brightness appear to be related by a power law. Our analysis shows that AIA observed flare brightness in UV 1600 Å relative to the quiescent brightness is a meaningful measurement of the flare chromosphere photometry. AIA observations for over a decade thus provide a unique and extensive database for systematic and semi-quantitative study of flaring chromosphere, either in the context of the Sun as a star, or in spatially resolved manner that helps to probe the nature of flare energy release on elementary scales.

利用AIA观测在1600 Å和304 Å波段量化耀斑能量释放的色球响应
大气成像组件(AIA)对太阳低层大气的成像观测大多被用作背景,它们的定量信息被探索得很少。色球层对耀斑期间磁重联释放的能量反应迅速。此外,耀斑是多重能量释放事件的集合,可以在空间分辨色球观测中识别。本文对AIA观测到的18个耀斑在uv1600 Å和euv304 Å波段的相对光度进行了统计和半定量研究。在每个耀斑中,我们在UV 1600 Å图像中识别了数千个耀斑带像素,并测量了它们的亮度(每秒计数)和上升和衰减时间尺度,这表明了耀斑环路的加热特性。分析表明,明亮耀斑像素的峰值亮度大于静止亮度的10倍,在半上升时间小于2 min时呈现出鲜明的亮度曲线,随后在与上升时间相当的时间尺度上呈现出快速衰减的两阶段衰减,然后逐渐衰减。在UV 1600 Å和EUV 304 Å图像中发现的耀斑带像素在上升过程中表现出相似的时间分布,并且它们的峰值亮度似乎与幂律相关。我们的分析表明,AIA在UV 1600观测到的耀斑亮度Å相对于静止亮度是耀斑色球光度法的一个有意义的测量。因此,AIA十多年的观测为系统和半定量地研究耀斑色球提供了一个独特而广泛的数据库,无论是在太阳作为一颗恒星的背景下,还是在空间分辨的方式下,都有助于在基本尺度上探测耀斑能量释放的本质。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
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来源期刊
Solar Physics
Solar Physics 地学天文-天文与天体物理
CiteScore
5.10
自引率
17.90%
发文量
146
审稿时长
1 months
期刊介绍: Solar Physics was founded in 1967 and is the principal journal for the publication of the results of fundamental research on the Sun. The journal treats all aspects of solar physics, ranging from the internal structure of the Sun and its evolution to the outer corona and solar wind in interplanetary space. Papers on solar-terrestrial physics and on stellar research are also published when their results have a direct bearing on our understanding of the Sun.
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