标题： 粒状磁泡在太阳大气中浮现。III. 通往过渡区的路径 显示英文标题

标题： Emergence of granular-sized magnetic bubbles through the solar atmosphere. III. The path to the transition region

摘要： 我们首次研究了粒状尺寸的磁泡从太阳光球层穿过色球层进入过渡区及以上的上升过程。这些事件发生在2013年9月25日 NOAA 11850中的磁场浮现区域。当时，瑞典1米太阳望远镜与IRIS航天器之间进行了第一次联合观测活动。使用SST的CRISP光谱偏振仪同时观测了色球层的H$\alpha$ 656.28纳米和\ion{Ca}{2} 854.2纳米线以及光球层的\ion{Fe}{1} 630.25纳米线，达到了0."14的空间分辨率。与此同时，IRIS对该磁场浮现区域进行了四步密集扫描，分别在133纳米（C~{\scii }，过渡区），140纳米（\ion{Si}{4}，过渡区），279.6纳米（\ion{Mg}{2} k，核心，上部色球层）和283.2纳米（\ion{Mg}{2} k，翼，光球层）处获取了狭缝图像。 几条谱线的光谱分析由IRIS光谱仪在远紫外线和近紫外线范围内完成，我们使用了其中的\ion{Si}{4} 140.3 和\ion{Mg}{2} k 279.6 nm 线。 来自太阳动力学天文台大气成像组件的日冕图像被用来研究通量浮现事件可能的日冕特征。 Ortiz等人（2014）详细描述了小尺度浮现磁泡的光球和色球特性。 在这里，我们能够追踪这些结构直至过渡区。 我们描述了所有层次观测到的通量浮现的特性，包括时间延迟。 我们认为这可能是从次表面层向过渡区和日冕输送能量和磁通量的一个重要机制。 显示英文摘要

摘要： We study the ascent of granular-sized magnetic bubbles from the solar photosphere through the chromosphere into the transition region and above, for the first time. Such events occurred in a flux emerging region in NOAA 11850 on September 25, 2013. During that time, the first co-observing campaign between the Swedish 1-m Solar Telescope and the IRIS spacecraft was carried out. Simultaneous observations of the chromospheric H$\alpha$ 656.28 nm and \ion{Ca}{2} 854.2 nm lines, plus the photospheric \ion{Fe}{1} 630.25 nm line, were made with the CRISP spectropolarimeter at the SST reaching a spatial resolution of 0."14. At the same time, IRIS was performing a four-step dense raster of the said emerging flux region, taking slit-jaw images at 133 (C~{\sc ii}, transition region), 140 (\ion{Si}{4}, transition region), 279.6 (\ion{Mg}{2} k, core, upper chromosphere), and 283.2 nm (\ion{Mg}{2} k, wing, photosphere). Spectroscopy of several lines was performed by the IRIS spectrograph in the far and near ultraviolet, of which we have used the \ion{Si}{4} 140.3 and the \ion{Mg}{2} k 279.6 nm lines. Coronal images from the Atmospheric Imaging Assembly of the Solar Dynamics Observatory were used to investigate the possible coronal signatures of the flux emergence events. The photospheric and chromospheric properties of small-scale emerging magnetic bubbles have been described in detail in Ortiz et al. (2014). Here we are able to follow such structures up to the transition region. We describe the properties, including temporal delays, of the observed flux emergence in all layers. We believe this may be an important mechanism of transporting energy and magnetic flux from subsurface layers to the transition region and corona.