We present comprehensive observations of the formation and evolution of a filament channel within NOAA Active Region (AR) 10978 from Hinode/Solar Optical Telescope and TRACE. We employ sequences of Hinode spectro-polarimeter maps of the AR, accompanying Hinode Narrowband Filter Instrument magnetograms in the Na I D1 line, Hinode Broadband Filter Instrument filtergrams in the Ca II H line and G-band, Hinode X-ray telescope X-ray images, and TRACE Fe IX 171?? image sequences. The development of the channel resembles qualitatively that presented by Okamoto et al. in that many indicators point to the emergence of a pre-existing sub-surface magnetic flux rope. The consolidation of the filament channel into a coherent structure takes place rapidly during the course of a few hours, and the filament form then gradually shrinks in width over the following two days. Particular to this filament channel is the observation of a segment along its length of horizontal, weak (500 G) flux that, unlike the rest of the filament channel, is not immediately flanked by strong vertical plage fields of opposite polarity on each side of the filament. Because this isolated horizontal field is observed in photospheric lines, we infer that it is unlikely that the channel formed as a result of reconnection in the corona, but the low values of inferred magnetic fill fraction along the entire length of the filament channel suggest that the bulk of the field resides somewhat above the low photosphere. Correlation tracking of granulation in the G band presents no evidence for either systematic flows toward the channel or systematic shear flows along it. The absence of these flows, along with other indications of these data from multiple sources, reinforces (but does not conclusively demonstrate) the picture of an emerging flux rope as the origin of this AR filament channel.
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机译：我们提出了从Hinode / Solar Optical Telescope和TRACE对NOAA活动区（AR）10978内的细丝通道形成和演化的全面观察。我们使用AR的Hinode光谱-极化仪图序列，Na I D1线随附的Hinode窄带滤光仪磁图，Ca II H线和G波段的Hinode宽带滤光仪滤镜图，Hinode X射线望远镜X射线图像和TRACE Fe IX 171？图像序列。该通道的发展在本质上与冈本等人的研究相似。其中许多指标指出了预先存在的地下磁通量绳索的出现。灯丝通道在数小时内迅速固结成紧密的结构，然后在接下来的两天内，灯丝形式的宽度逐渐缩小。对此长丝通道的特别之处是沿其水平弱（500 G）通量的长度观察到一段，与其余长丝通道不同，该通量没有立即在两侧的极性相反的强垂直杂波场侧接灯丝。因为在光球线中观察到了这种孤立的水平场，所以我们推断出由于电晕中的重新连接而形成的通道的可能性不大，但是沿灯丝通道的整个长度推断出的磁性填充率较低，这表明大部分视场都位于低光圈上方。在G带中的颗粒的相关性跟踪没有证据表明向通道的系统流动或沿通道的系统剪切流动。这些流量的缺乏，以及来自多个来源的这些数据的其他指示，都增强了（但未最终证明）作为该AR灯丝通道起源的助焊剂绳索的情况。
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