Detecting the Oscillation and Propagation of the Nascent Dynamic Solar Wind Structure at 2.6 Solar Radii Using Very Long Baseline Interferometry Radio Telescopes
Detecting the Oscillation and Propagation of the Nascent Dynamic Solar Wind Structure at 2.6 Solar Radii Using Very Long Baseline Interferometry Radio Telescopes
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使用甚长基线干涉射电望远镜检测 2.6 个太阳半径处新生动态太阳风结构的振荡和传播
DOI：
10.3847/2041-8213/ac96e7
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发表时间：
2022
影响因子：
7.9
通讯作者：
Yingkai Li
中科院分区：
文献类型：
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作者：
Maoli Ma;Guifré Molera Calvés;Giuseppe Cimò;Ming Xiong;Peijia Li;Jing Kong;Peijin Zhang;Jiansen He;Lijia Liu;Pradyumna Kummamuru;Chuanpeng Hou;Jasper Edwards;Qinghui Liu;Zhong Chen;Zhanghu Chu;De Wu;Xu Zhao;Zhichao Wang;Songtao Han;Quanquan Zhi;Yingkai Li
抽象的。日冕探测是研究日冕加热和太阳风加速的关键。然而，瞬态和不均匀的太阳风流动携带大振幅的固有阿尔文波和湍流，这使得检测更加困难。利用中国天文台和欧洲航天局火星快车射电望远镜的观测资料，报道了太阳风在2.6太阳半径（Rs）处的振荡和传播。这些观测是在2021年10月9日进行的，当时一个日冕物质抛射（CME）穿过望远镜光束的射线路径。我们得到的频率波动（FFs）的航天器信号从每个单独的望远镜。首先，我们以高空间分辨率沿投影基线沿着数千公里的频率尖峰的漂移进行视觉识别。它们被用作估计太阳风速度的轨迹。然后对不同望远镜观测到的FF时间序列进行互相关分析。得到了CME通过过程中太阳风结构沿着径向和切向的速度变化。切向速度的振荡证实了流光波的检测。此外，在CME的尾部，我们检测到一个加速的快速场排列的密度结构的传播，表明磁流体动力学波的存在。这项研究证实，地面站对能够形成特定的空间投影基线，具有高分辨率和灵敏度，以研究新生的动态太阳风结构的详细传播。
Abstract. Probing the solar corona is crucial to study the coronal heating and solar wind acceleration. However, the transient and inhomogeneous solar wind flows carry large-amplitude inherent Alfvén waves and turbulence, which make detection more difficult. We report the oscillation and propagation of the solar wind at 2.6 solar radii (Rs) by observation of China’s Tianwen and ESA’s Mars Express with radio telescopes. The observations were carried out on 2021 October 9, when one coronal mass ejection (CME) passed across the ray paths of the telescope beams. We obtain the frequency fluctuations (FFs) of the spacecraft signals from each individual telescope. First, we visually identify the drift of the frequency spikes at a high spatial resolution of thousands of kilometers along the projected baselines. They are used as traces to estimate the solar wind velocity. Then we perform the cross-correlation analysis on the time series of FF from different telescopes. The velocity variations of solar wind structure along radial and tangential directions during the CME passage are obtained. The oscillation of tangential velocity confirms the detection of a streamer wave. Moreover, at the tail of the CME, we detect the propagation of an accelerating fast field-aligned density structure indicating the presence of magnetohydrodynamic waves. This study confirms that the ground-station pairs are able to form particular spatial projection baselines with high resolution and sensitivity to study the detailed propagation of the nascent dynamic solar wind structure.