带光桥的太阳孔的光球环境
The photospheric environment of a solar pore with light bridge
摘要：
太阳表面出现磁场，在光球层中形成各种特征，其中之一就是孔隙。它们位于微小的磁性元素和较大的太阳黑子之间的边界。光桥，在这样的结构中，是明亮的特征，将阴影区域分隔成两个或多个不规则区域。通常，光桥表明磁性区域的合并，或者相反，该区域的分裂正在进行中。我们研究了带有光桥的太阳孔（AR 10812）和附近安静的太阳光球的速度结构，分析了高空间和光谱分辨率的图像。孔面积已观察到与干涉双维光谱仪（IBIS）在邓恩太阳望远镜，获取单色图像在Ca II 854.2 nm线和Fe I 709.0 nm线，以及G-波段和宽带图像。我们还计算了与Fe I和Fe II光球线相关的视线（LoS）速度场。的LoS速度波动的幅度，孔内，是小于所观察到的安静的造粒附近的活动区域。我们计算了方位平均LoS速度，并推导出其径向轮廓。整个孔隙的特征是向下速度为-200 m/s，相对于附近的安静太阳，环形向下流动结构的平均速度为-350 m/s。孔内的光桥，当观察到的宽带通道的IBIS和钙II 854.2 nm线的红翼，显示了一个细长的黑暗结构沿其轴运行，我们解释与半解析模型。在最高分辨率的LoS速度图像中，光桥显示出与对流卷一致的轮廓：弱的上升流，50- 100 m/s，对应于暗巷，两侧是下降流，-（200-300）m/s。
英文摘要：
Pores are one of the various features forming in the photosphere by the emergence of magnetic field onto the solar surface. They lie at the border between tiny magnetic elements and larger sunspots. Light bridges, in such structures, are bright features separating umbral areas in two or more irregular regions. Commonly, light bridges indicate that a the merging of magnetic regions or, conversely, the breakup of the area is underway. We investigate the velocity structure of a solar pore (AR10812) with light bridge, and of the quiet solar photosphere nearby, analyzing high spatial and spectral resolution images. The pore area has been observed with the Interferometric BI-dimensional Spectrometer (IBIS) at the Dunn Solar Telescope, acquiring monochromatic images in the Ca II 854.2 nm line and in the Fe I 709.0 nm line as well as G-band and broad-band images. We also computed the Line of Sight (LoS) velocity field associated to the Fe I and Fe II photospheric lines. The amplitude of the LoS velocity fluctuations, inside the pore, is smaller than that observed in the quiet granulation near the active region. We computed the azimuthal average LoS velocity and derived its radial profile. The whole pore is characterized by a downward velocity -200 m/s and by an annular downflow structure with an average velocity of -350 m/s with respect to the nearby quiet sun. The light bridge inside the pore, when observed in the broad-band channel of IBIS and in the red wing of Ca II 854.2 nm line, shows an elongated dark structure running along its axis, that we explain with a semi-analytical model. In the highest resolution LoS velocity images the light bridge shows a profile consistent with a convective roll: a weak upflow, 50-100m/s, in correspondence of the dark lane, flanked by a downflow, -(200-300) m/s.
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