DETERMINATION OF SUB-RESOLUTION STRUCTURE OF A JET BY SOLAR MAGNETOSEISMOLOGY
DETERMINATION OF SUB-RESOLUTION STRUCTURE OF A JET BY SOLAR MAGNETOSEISMOLOGY
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DOI：
10.1088/0004-637x/744/1/5
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发表时间：
2011-09
期刊：
影响因子：
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通讯作者：
R. Morton;G. Verth;J. McLaughlin;R. Erd'elyi
中科院分区：
文献类型：
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作者：
R. Morton;G. Verth;J. McLaughlin;R. Erd'elyi
在171？、193？和211？的UV/EUV太阳喷流中观察到一条细长的暗线，部分在304？中观察到。暗线似乎起源于色球，但它的温度似乎不在太阳动力学天文台上大气成像组件的通带范围内。因此，我们利用太阳磁震学来估计暗线的等离子体参数。观察到一个正在传播的扭结(横向)波沿着暗线传播。通过沿着暗线的轴线放置多个狭缝，可以在∼7000公里的范围内跟踪波。估计了波的相速度和振幅，并利用磁震学理论确定了等离子体参数。我们能够估计暗线的等离子体温度、密度梯度、磁场梯度和亚分辨率展开。发现暗线很冷，T≲为3×10~4，具有很强的密度和磁场梯度。通量管沿其长度的膨胀为∼300-400公里。
A thin dark thread is observed in a UV/EUV solar jet in the 171 Å, 193 Å, and 211 Å, and partially in 304 Å. The dark thread appears to originate in the chromosphere but its temperature does not appear to lie within the passbands of the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory. We therefore implement solar magnetoseismology to estimate the plasma parameters of the dark thread. A propagating kink (transverse) wave is observed to travel along the dark thread. The wave is tracked over a range of ∼7000 km by placing multiple slits along the axis of the dark thread. The phase speed and amplitude of the wave are estimated and magnetoseismological theory is employed to determine the plasma parameters. We are able to estimate the plasma temperature, density gradient, magnetic field gradient, and sub-resolution expansion of the dark thread. The dark thread is found to be cool, T ≲ 3 × 104, with both strong density and magnetic field gradients. The expansion of the flux tube along its length is ∼300–400 km.