He I 10830年太阳系中弓形丝状体的时间演化
Temporal evolution of arch filaments as seen in He I 10830 Å
摘要：
我们研究了弓丝系统（AFS）及其单个弓丝的演变，以了解它们中发生的过程。我们在特内里费岛的格里戈尔太阳望远镜上用格里戈尔红外光谱仪（GRIS）的非常快的光谱模式在He I 10830 nm光谱范围内以高节奏观测了AFS。He I三重态配置文件与解析函数拟合，以推断视线（LOS）速度，以遵循AFS内的等离子体运动。我们跟踪了单个弓丝在其整个生命周期中的时间演化，如He I 10830 π三联体所示。弓丝高度膨胀，长度从13”延伸到21”。在He I中看到弓丝后约11 min，环顶开始上升，平均多普勒速度为6 km/s。仅仅两分钟后，等离子体就以超音速流向足点，在色球层中达到高达40 km/s的峰值速度。He I 10830配置文件附近的领先孔的时间演变显示几乎无处不在的双红色分量的He I三重态，表明强大的下行流，随着材料几乎在同一分辨率的元素在整个观察时间内休息。我们跟随着拱形灯丝，因为它在从光球上升到日冕的过程中携带着等离子体。然后，物质沿着拱形灯丝的腿部流向光球，达到超音速。我们的观测结果支持理论AFS模型，并有助于改善未来的模型。
英文摘要：
We study the evolution of an arch filament system (AFS) and of its individual arch filaments to learn about the processes occurring in them. We observed the AFS at the GREGOR solar telescope on Tenerife at high cadence with the very fast spectroscopic mode of the GREGOR Infrared Spectrograph (GRIS) in the He I 10830 Å spectral range. The He I triplet profiles were fitted with analytic functions to infer line-of-sight (LOS) velocities to follow plasma motions within the AFS. We tracked the temporal evolution of an individual arch filament over its entire lifetime, as seen in the He I 10830 Å triplet. The arch filament expanded in height and extended in length from 13" to 21". The lifetime of this arch filament is about 30 min. About 11 min after the arch filament is seen in He I, the loop top starts to rise with an average Doppler velocity of 6 km/s. Only two minutes later, plasma drains down with supersonic velocities towards the footpoints reaching a peak velocity of up to 40 km/s in the chromosphere. The temporal evolution of He I 10830 Å profiles near the leading pore showed almost ubiquitous dual red components of the He I triplet, indicating strong downflows, along with material nearly at rest within the same resolution element during the whole observing time. We followed the arch filament as it carried plasma during its rise from the photosphere to the corona. The material then drained toward the photosphere, reaching supersonic velocities, along the legs of the arch filament. Our observational results support theoretical AFS models and aids in improving future models.
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