论文标题
在太阳的阿尔玛单次图像中检测到的耀斑
Flares detected in ALMA single-dish images of the Sun
论文作者
论文摘要
太阳耀斑的（子）毫米辐射知之甚少。没有空间分辨率，就无法轻松比较其他波长中的耀斑排放。 ATACAMA大毫米毫米阵列（ALMA）首次提供足够的分辨率。但是，用作干涉仪，其视野小于活性区域，而阿尔玛（Alma）在发生耀斑时无法按需观察。我们使用易于使用的太阳毫米耀斑的大规模单次ALMA观测值，并将它们与其他波长中观察到的知名特征进行比较。然后，这些其他耀斑排放的特性，与时空相关，然后可以用来解释毫米亮丽，反之亦然。目的是获得可靠的关联，受单次观察的时间和空间分辨率的限制。我们以3毫米和1毫米的速度收集了ALMA观测值，并在耀斑目录中给出的时间搜索了毫米亮丽。我们发现了五个具有9个或更多图像的事件，可用于比较时间和空间。毫米光泽与凉爽（H $α$，30.4 nm），中级（17.1 nm）和热（9.4 nm）线的各种耀斑特征有关。在某些情况下，毫米亮度在热耀斑环的脚上达到顶峰。在其他情况下，峰与活性Hα细丝的顶部或脚部重合。我们发现了与热循环后的循环和顶部的相关性，在某些情况下根本没有功能。单次观察提供的广泛视野允许首次完全概述毫米波的耀斑活动。相关的现象经常在类型和位置的耀斑期间发生变化，并且可以解释以前在没有空间分辨率的情况下观察到的毫米耀斑排放的有时令人困惑的行为。
The (sub)millimeter radiation of solar flares is poorly understood. Without spatial resolution, it cannot be compared easily to flare emissions in other wavelengths. The Atacama Large Millimeter-submillimeter Array (ALMA) offers sufficient resolution for the first time. However, used as an interferometer, its field of view is smaller than an active region and ALMA cannot observe on demand when a flare occurs. We use readily available large scale single-dish ALMA observations of solar millimeter flares and compare them to well-known features observed in other wavelengths. The properties of these other flare emissions, correlating in space and time, may then be used to interpret the millimeter brightenings and vice versa. The aim is to obtain reliable associations, limited by the time and space resolution of single-dish observations. We collected ALMA observations at 3 mm and 1 mm and searched for millimeter brightenings during times given in a flare catalog. We found five events with 9 or more images that can be used for comparison in time and space. The millimeter brightenings are associated with a variety of flare features in cool (H$α$, 30.4 nm), intermediate (17.1 nm), and hot (9.4 nm) lines. In several cases, the millimeter brightening peaked at the footpoint of a hot flare loop. In other cases the peak coincided with the top or footpoint of an active Hα filament. We found correlations also with post-flare loops and tops of a hot loop, and in some cases to no features at all. The wide field of view provided by the single-dish observations allowed for completely overviewing the flare activity in millimeter waves for the first time. The associated phenomena often changed during the flare in type and location, and may explain the sometimes bewildering behavior of millimeter flare emissions observed previously without spatial resolution.
