Observations of a Quasi-periodic, Fast-Propagating Magnetosonic Wave in Multiple Wavelengths and Its Interaction with Other Magnetic Structures
Observations of a Quasi-periodic, Fast-Propagating Magnetosonic Wave in Multiple Wavelengths and Its Interaction with Other Magnetic Structures
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多波长准周期、快速传播的磁声波及其与其他磁结构相互作用的观测
DOI：
10.1007/s11207-013-0395-4
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发表时间：
2013-07
期刊：
影响因子：
2.8
通讯作者：
Elmhamdi, A.
中科院分区：
文献类型：
--
作者：
Shen, Y. -D.;Liu, Y.;Su, J. -T.;Li, H.;Zhang, X. -F.;Tian, Z. -J.;Zhao, R. -J.;Elmhamdi, A.
我们目前的观测准周期快速传播（QFP）磁声波2012年4月23日，与高分辨率的观测大气成像组件机载太阳动力学天文台。在一次C2.0耀斑开始后3分钟，在距引导环系统足点150 Mm、速度为689 km/s的171个观测点中，首先观测到波列沿沿着一个开放发散环系统运动，然后在193个观测点中，波列在与路径上一个垂直的下伏环系统相互作用后出现;速度在短时间内降到343公里/秒。波列的突然减速和它们在193个观测中的出现分别通过几何效应和引导环系统的密度增加来解释。我们发现波列与耀斑有80秒的共同周期。此外，在QFP波中还识别出了一些低频。我们认为80秒周期的产生是由于磁场重联过程中的非线性能量爆发的周期性释放造成的，而低频可能是光球层或色球层的压力驱动振荡的泄漏，这可能是驱动日冕QFP波的一个重要来源。我们的研究结果还表明，引导磁结构的性质，如磁场和密度的分布以及几何形状，是至关重要的调制QFP波的传播行为。
We present observations of a quasi-periodic fast-propagating (QFP) magnetosonic wave on 23 April 2012, with high-resolution observations taken by the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory. Three minutes after the start of a C2.0 flare, wave trains were first observed along an open divergent loop system in 171 Å observations at a distance of 150 Mm from the footpoint of the guiding loop system and with a speed of 689 km s−1, then they appeared in 193 Å observations after their interaction with a perpendicular, underlaying loop system on the path; in the meantime; their speed decelerated to 343 km s−1 within a short time. The sudden deceleration of the wave trains and their appearance in 193 Å observations are interpreted through a geometric effect and the density increase of the guiding loop system, respectively. We find that the wave trains have a common period of 80 seconds with the flare. In addition, a few low frequencies are also identified in the QFP wave. We propose that the generation of the period of 80 seconds was caused by the periodic releasing of energy bursts through some nonlinear processes in magnetic reconnection, while the low frequencies were possibly the leakage of pressure-driven oscillations from the photosphere or chromosphere, which could be an important source for driving coronal QFP waves. Our results also indicate that the properties of the guiding magnetic structure, such as the distributions of magnetic field and density as well as geometry, are crucial for modulating the propagation behaviors of QFP waves.
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影响因子：
10.3
作者：
M. Kuperus
通讯作者：
M. Kuperus
影响因子：
33.3
作者：
G. Withbroe;R. Noyes
通讯作者：
G. Withbroe;R. Noyes
影响因子：
20.9
作者：
V. Nakariakov;E. Verwichte
通讯作者：
V. Nakariakov;E. Verwichte
影响因子：
2.8
作者：
W. Pesnell;B. Thompson;P. Chamberlin
通讯作者：
W. Pesnell;B. Thompson;P. Chamberlin
DOI：
10.1086/147165
发表时间：
1961-09
期刊：
The Astrophysical Journal
影响因子：
--
作者：
D. Osterbrock
通讯作者：
D. Osterbrock