论文标题
在太阳能拱形系统中跟踪从色球到光球的下流流量
Tracking downflows from the chromosphere to the photosphere in a solar arch filament system
论文作者
论文摘要
我们研究了从圆形系统到光球沿拱形系统（AFS）的血浆的动力学，并从两个基于地面的太阳能望远镜的高效率光谱数据观察到，使用Gregor望远镜（Tenerife）使用Gregor Inderpraught（Gris）在He I 10830Å范围内使用Gregor Indermant（Tenerife）（Tenerife）。成像光谱仪观察Ca II8542Å和Fe I6173Å光谱线。等离子体的排水的时间演变沿着从色球球到光球的单个拱形丝的腿沿着单个拱形丝的腿进行。从He I I10830Å三重速度到达20-24〜 km〜s $^{ - 1} $的平均多普勒速度，在下色层和上部光球上，多普勒的速度最高为11〜 km〜s $^s $^{ - 1} $ 1.5 km〜s.5 km〜 8542Å和Si I10827Å光谱线。多普勒速度在太阳大气的不同层（染色体和上光球）处的演变表明，它们遵循相同的LOS速度模式，这证实了观察性证据表明，血浆与AFSS模型中所提出的光泽朝向光球。从较低的光电CA I10839Å或Fe I6173Å光谱线推断出的多普勒速度图不会显示相同的LOS速度模式。因此，没有证据表明血浆到达较低的光球。观测值和非线力场外推表明，AFS的磁场环随时间上升。我们在AFS的不同脚步处发现流动不对称。磁场强度的NLFFF值为我们提供了解释这些流动不对称的线索。
We study the dynamics of plasma along the legs of an arch filament system (AFS) from the chromosphere to the photosphere, observed with high-cadence spectroscopic data from two ground-based solar telescopes: the GREGOR telescope (Tenerife) using the GREGOR Infrarred Spectrograph (GRIS) in the He I 10830 Å range and the Swedish Solar Telescope (La Palma) using the CRisp Imaging Spectro-Polarimeter to observe the Ca II 8542 Å and Fe I 6173 Å spectral lines. The temporal evolution of the draining of the plasma was followed along the legs of a single arch filament from the chromosphere to the photosphere. The average Doppler velocities inferred at the upper chromosphere from the He I 10830 Å triplet reach velocities up to 20-24~km~s$^{-1}$, in the lower chromosphere and upper photosphere the Doppler velocities reach up to 11~km~s$^{-1}$ and 1.5~km~s$^{-1}$ in the case of the Ca II 8542 Å and Si I 10827 Å spectral lines, respectively. The evolution of the Doppler velocities at different layers of the solar atmosphere (chromosphere and upper photosphere) shows that they follow the same LOS velocity pattern, which confirm the observational evidence that the plasma drains towards the photosphere as proposed in models of AFSs. The Doppler velocity maps inferred from the lower photospheric Ca I 10839 Å or Fe I 6173 Å spectral lines do not show the same LOS velocity pattern. Thus, there is no evidence that the plasma reaches the lower photosphere. The observations and the nonlinear force-free field extrapolations demonstrate that the magnetic field loops of the AFS rise with time. We found flow asymmetries at different footpoints of the AFS. The NLFFF values of the magnetic field strength give us a clue to explain these flow asymmetries.
