Dynamics of Subarcsecond Bright Dots in the Transition Region above Sunspots and Their Relation to Penumbral Micro-jets
Dynamics of Subarcsecond Bright Dots in the Transition Region above Sunspots and Their Relation to Penumbral Micro-jets
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太阳黑子上方过渡区亚弧秒亮点的动力学及其与半影微喷流的关系
DOI：
10.3847/2041-8213/835/2/l19
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发表时间：
2017-01
影响因子：
7.9
通讯作者：
Schanche Nicole
中科院分区：
文献类型：
--
作者：
Samanta Tanmoy;Tian Hui;Banerjee Dipankar;Schanche Nicole
最近的高分辨率观测显示，在太阳黑子半影上方的过渡区，普遍存在着寿命低于分钟的亚弧秒亮点(BDS)。此前有报道称，色球中存在半影微喷流(PMJ)。认为PMJ和BDS都是由于磁重联过程而形成的，可能在半影的加热过程中起着重要作用。利用Hinode上太阳光学望远镜(SOT)对色球的同步观测和界面区成像光谱仪对色球的观测，我们研究了BDS的动力学及其与PMJ的关系。我们发现了两种类型的BDS，一种与PMJ有关，另一种在SOT Ca II H图像中没有显示任何可见的动态。从统计分析可以看出，这两种类型具有不同的性质。与PMJ相关的BDS总是出现在PMJ的顶端，绝大多数都是向内运动的，起源于PMJ的生成之前。这些结果可能表明重联发生在较低的日冕/tr高度，并在色球启动PMJ。这种形成机制与在不同倾斜场之间的(上层)光球层重联形成PMJ形成相反。
Recent high-resolution observations have revealed that subarcsecond bright dots (BDs) with sub-minute lifetimes appear ubiquitously in the transition region (TR) above sunspot penumbra. The presence of penumbral micro-jets (PMJs) in the chromosphere was previously reported. It was proposed that both the PMJs and BDs are formed due to a magnetic reconnection process and may play an important role in heating of the penumbra. Using simultaneous observations of the chromosphere from the Solar Optical Telescope (SOT) on board Hinode and observations of the TR from the Interface Region Imaging Spectrograph, we study the dynamics of BDs and their relation to PMJs. We find two types of BDs, one that is related to PMJs, and another that does not show any visible dynamics in the SOT Ca ii H images. From a statistical analysis we show that these two types have different properties. The BDs that are related to PMJs always appear at the top of the PMJs, the vast majority of which show inward motion and originate before the generation of the PMJs. These results may indicate that the reconnection occurs at the lower coronal/TR height and initiates PMJs at the chromosphere. This formation mechanism is in contrast with the formation of PMJs by reconnection in the (upper) photosphere between differently inclined fields.
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DOI：
10.1051/0004-6361/201527340
发表时间：
2015-12
期刊：
arXiv: Solar and Stellar Astrophysics
影响因子：
--
作者：
L. P. Chitta;H. Peter;P. Young;P. Young
通讯作者：
L. P. Chitta;H. Peter;P. Young;P. Young
DOI：
10.3847/0004-637x/822/1/35
发表时间：
2016-03
期刊：
The Astrophysical Journal
影响因子：
--
作者：
S. E. Alpert;S. Tiwari;R. Moore;A. Winebarger;S. Savage
通讯作者：
S. E. Alpert;S. Tiwari;R. Moore;A. Winebarger;S. Savage
影响因子：
6.5
作者：
V. Henriques;D. Kiselman
通讯作者：
V. Henriques;D. Kiselman
影响因子：
6.5
作者：
L. B. Rubio;H. Balthasar;M. Collados
通讯作者：
L. B. Rubio;H. Balthasar;M. Collados
DOI：
10.1086/173450
发表时间：
1993-12
期刊：
The Astrophysical Journal
影响因子：
--
作者：
B. Lites;D. Elmore;P. Seagraves;A. Skumanich
通讯作者：
B. Lites;D. Elmore;P. Seagraves;A. Skumanich