半影区微射流的多诊断谱分析
A multi-diagnostic spectral analysis of penumbral microjets
摘要：
半影微喷流（PMJ）是在太阳黑子半影中发现的短暂的喷流状物体。它们首先在色球谱线中被发现，后来也被证明在过渡区（TR）谱线中显示出信号。它们的起源和演化方式尚未确定。我们进行了全面的分析PMJ通过使用光谱诊断，跨度从光球TR温度，以约束PMJ属性。我们采用了高空间分辨率的瑞典1米太阳望远镜对Ca II 8542埃和H-α线的观测，IRIS狭缝颚图像，以及IRIS对Mg II h & k线、Mg II 2798.75埃和2798.82埃三重态混合线、C II 1334埃和1335埃线的光谱观测，以及Si IV 1394埃和1403埃线。我们从这些光谱诊断中得到了广泛的范围，并研究了与PMJ相关的其他次级现象。我们发现PMJ在我们研究的所有谱线中表现出不同程度的信号。我们发现低或可忽略的多普勒速度和速度梯度在我们的诊断和所有层的太阳大气与这些相关。H-α和Ca II 8542埃的内翼中的深色特征意味着PMJ沿着预先存在的原纤维结构形成。我们发现的证据，上层光球加热PMJ的一个子集，通过在机翼上的Mg II三线发射。几乎没有证据表明PMJ中普遍存在扭转运动。不同谱线PMJ增亮的起始时间无明显差异。PMJ最有可能只表现出非常温和的质量运动，与早期的建议相反。我们认为PMJ形成于光球层或色球层的上部，在预先存在的纤维结构中。
英文摘要：
Penumbral microjets (PMJs) are short-lived, jet-like objects found in the penumbra of sunspots. They were first discovered in chromospheric lines and have later also been shown to exhibit signals in transition region (TR) lines. Their origin and manner of evolution is not yet settled. We perform a comprehensive analysis of PMJs through the use of spectral diagnostics that span from photospheric to TR temperatures to constrain PMJ properties. We employed high-spatial-resolution Swedish 1-m Solar Telescope observations in the Ca II 8542 Angstrom and H-alpha lines, IRIS slit-jaw images, and IRIS spectral observations in the Mg II h & k lines, the Mg II 2798.75 Angstrom & 2798.82 Angstrom triplet blend, the C II 1334 Angstrom & 1335 Angstrom lines, and the Si IV 1394 Angstrom & 1403 Angstrom lines. We derived a wide range of spectral diagnostics from these and investigated other secondary phenomena associated with PMJs. We find that PMJs exhibit varying degrees of signal in all of our studied spectral lines. We find low or negligible Doppler velocities and velocity gradients throughout our diagnostics and all layers of the solar atmosphere associated with these. Dark features in the inner wings of H-alpha and Ca II 8542 Angstrom imply that PMJs form along pre-existing fibril structures. We find evidence for upper photospheric heating in a subset of PMJs through emission in the wings of the Mg II triplet lines. There is little evidence for ubiquitous twisting motion in PMJs. There is no marked difference in onset-times for PMJ brightenings in different spectral lines. PMJs most likely exhibit only very modest mass-motions, contrary to earlier suggestions. We posit that PMJs form at upper photospheric or chromospheric heights at pre-existing fibril structures.
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