A Study of a Tiny Two-Ribbon Flare Driven by Emerging Flux
A Study of a Tiny Two-Ribbon Flare Driven by Emerging Flux
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DOI：
10.1086/424823
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发表时间：
2004-11
期刊：
影响因子：
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通讯作者：
Takuma Sakajiri;D. Brooks;Tetsuya T. Yamamoto;D. Shiota;H. Isobe;S. Akiyama;S. Ueno;R. Kitai;K. Shibata
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文献类型：
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作者：
Takuma Sakajiri;D. Brooks;Tetsuya T. Yamamoto;D. Shiota;H. Isobe;S. Akiyama;S. Ueno;R. Kitai;K. Shibata
我们介绍了2001年7月14日发生在NOAA 9537活动区附近的微型细丝喷发的观测结果。此次喷发由飞驒天文台无圆顶太阳望远镜（Hα线中心和±0.4 Å翼）、太阳和日光层天文台EUV成像望远镜（EIT）和迈克尔逊多普勒成像仪以及Yohkoh软x射线望远镜（SXT）观测。微型细丝开始形成，并在06:50 UT左右在Hα图像中清晰可见。大约25分钟后，它爆发了，伴随着一个小的双带状亚耀斑（面积为61弧秒2）。这两个条带也被发现以每秒3.33公里的速度接近对方。我们发现，这一事件是由一个安静区域出现新的磁通量引起的。在前一天拍摄的EIT和SXT图像中，新出现的通量显示为一个明亮的区域。它向南移动到先前存在的相反极性通量的区域，在那里形成了一个抵消磁通量的区域。微细丝随后出现，我们认为它通过延迟新出现的和先前存在的通量之间的重新连接来抑制能量的释放，正如在EUV和软x射线图像中相反极性之间的明亮区域消失所证明的那样。因此，磁能是两个相反极性通量区（0.17 km s-1）缓慢汇聚运动的结果。灯丝下方的重新连接引起了灯丝的喷发，并发生了双带状耀斑。微型细丝被认为是大型细丝的小型类似物。我们的观察还表明，小规模耀斑和大规模耀斑之间存在一些共同的特性。这些结果支持这样一种观点，即统一的磁重联模型可能能够解释所有规模的耀斑。
We present observations of the eruption of a miniature filament that occurred near NOAA Active Region 9537 on 2001 July 14. The eruption was observed by the Hida Observatory Domeless Solar Telescope, in the Hα line center and ±0.4 Å wings, the Solar and Heliospheric Observatory EUV Imaging Telescope (EIT) and Michelson Doppler Imager, and the Yohkoh Soft X-Ray Telescope (SXT). The miniature filament began to form and was clearly visible in Hα images by around 06:50 UT. It erupted about 25 minutes later, accompanied by a small two-ribbon subflare (with an area of 61 arcsec2). The two ribbons were also found to approach each other at a speed of 3.33 km s-1. We found that this event was caused by the emergence of new magnetic flux in a quiet region. The emerging flux appeared as a bright region in the EIT and SXT images taken on the previous day. It moved southward into an area of preexisting opposite-polarity flux, where a cancelling magnetic flux region was formed. The miniature filament then appeared, and we suggest that it played some role in inhibiting the release of energy by delaying reconnection between the emerging and preexisting flux, as evidenced by the disappearance of the bright region between opposite polarities in the EUV and soft X-ray images. Consequently, magnetic energy was stored as a result of the slow converging motion of the two opposite-polarity flux regions (0.17 km s-1). Reconnection below the filament provoked the filament eruption, and the two-ribbon flare occurred. Miniature filaments are thought to be small-scale analogs of large-scale filaments. Our observations also suggest some common properties between small-scale and large-scale flares. These results support the view that a unified magnetic reconnection model may be able to explain all scales of flares.