Observations of Chromospheric Anemone Jets with Hinode Ca II Broadband Filtergraph and Hida Ca II Spectroheliograph
Observations of Chromospheric Anemone Jets with Hinode Ca II Broadband Filtergraph and Hida Ca II Spectroheliograph
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DOI：
10.1093/pasj/62.4.901
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发表时间：
2010-02
影响因子：
2.3
通讯作者：
S. Morita;K. Shibata;S. Ueno;K. Ichimoto;R. Kitai;Ken Otsuji
中科院分区：
文献类型：
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作者：
S. Morita;K. Shibata;S. Ueno;K. Ichimoto;R. Kitai;Ken Otsuji
本文报道了利用希达天文台的日之出太阳光学望远镜（SOT）Ca Ⅱ H宽带滤波器和圆顶太阳望远镜（DST）上的Ca Ⅱ K分光日像仪首次同时观测到的太阳活动区色球“海葵”喷流。在协调观测期间，用这两台仪器同时观测了9个色球海葵喷流。这些观测揭示了三个重要特征：（1）喷流产生于色球层下部;即，（2）喷流的长度和寿命分别为0.4-5 μ m和40-320 s;（3）用SOT观测到的喷流的视速度为3-24 km·s-1，而喷流处的Ca II K3分量显示出2-6 km·s-1范围内的蓝移（5次事件）。色球海葵喷流与混合极性区域有关，这些区域要么是小的新兴通量区域，要么是移动的磁性特征。发现Ca II K线在K2/K1分量中经常显示红色或蓝色的不对称性;与新兴通量区相关的喷流的足迹经常显示红移（2-16 km s-1），而具有移动磁特征的喷流的足迹则显示蓝移（-5 km s-1）。对喷流形成区域的磁演化的详细分析表明，总磁通量在喷流的足点（或抵消率）是在10 16 Mx s-1的顺序，和由此产生的磁能释放率是（1.1-10）× 10 24 erg s × 1，在磁抵消的持续时间内，总能量释放为（1-13）× 10 26 erg，× 130 s。这些与估计的总能量相当，在一个单一的色球海葵喷流中为1026尔格。除了DST Ca II K太阳光谱图和SOT Ca II H宽带滤波图外，我们还用SOT磁象图和希达H滤波图进行了分析。在此基础上提出了色球海葵喷流的物理模型，并讨论了色球海葵喷流与埃勒曼炸弹的关系。
We report on the first simultaneous observations of chromospheric “anemone” jets in solar active regions with the Hinode Solar Optical Telescope (SOT) Ca II H broadband filtergraph and the Ca II K spetroheliograph on the Domeless Solar Telescope (DST) at Hida Observatory. During the period of coordinated observations, nine chromospheric anemone jets were simultaneously observed with the two instruments. These observations revealed three important features: (1) the jets are generated in the lower chromosphere; i.e., these cannot be seen in Ca II K3 ;( 2) the length and lifetime of the jets are 0.4–5 Mm and 40–320 s, respectively; (3) the apparent velocity of the jets observed with the SOT is 3–24 km s � 1 , while the Ca II K3 component at the jets shows a blueshift (in 5 events) in the range of 2–6 km s � 1 . The chromospheric anemone jets are associated with mixed polarity regions, which are either small emerging flux regions or moving magnetic features. It is found that the Ca II K line often shows red or blue asymmetry in the K2/K1 component; the footpoint of the jets associated with emerging flux regions often shows a redshift (2–16 km s � 1 ), while the one with moving magnetic features shows a blueshift (� 5k m s � 1 ). A detailed analysis of the magnetic evolution of the jet-forming regions revealed that the reconnection rate (or canceling rate) of the total magnetic flux at the footpoint of the jets is on the order of 10 16 Mx s � 1 , and the resulting magnetic energy release rate is (1.1–10) � 10 24 erg s � 1 , with a total energy release of (1–13) � 10 26 erg for the duration of the magnetic cancellation, � 130 s. These are comparable to the estimated total energy, � 10 26 erg, in a single chromospheric anemone jet. In addition to the DST Ca II K spectroheliogram and the SOT Ca II H broadband filtergram, we also used for analysis an SOT magnetogram as well as a Hida H˛ filtergram. We present a physical model of the jet based on the observation, and discuss the relation between chromospheric anemone jets and Ellerman bombs.