太陽プロミネンスにおける逆流の起源を解明 (Researchers Uncover Origin of Counterstreaming Flows in Solar Prominences)

ad

2025-03-17 中国科学院(CAS)

中国科学院の研究チームは、太陽プロミネンスの動的進化に関する新たな発見を発表した。高解像度の1メートル新真空太陽望遠鏡(NVST)とNASAのIRIS衛星データを用い、プロミネンス内の逆流運動の起源を詳細に分析した。観測の結果、スパイン上部は83分周期の振動を示し、中部では秒速10~20kmの逆流、下部では断続的な物質注入が確認された。この物質の流れは、プルームの上昇運動と磁気トルネードの影響によるもので、逆流運動の形成に関与している。本研究は、プロミネンス内の運動メカニズムの理解を深める重要な成果である。

<関連情報>

太陽静止期プロミネンスにおける振動、対向流、質量注入の同時存在 Simultaneous Existence of Oscillations, Counterstreaming Flows, and Mass Injections in Solar Quiescent Prominences

Xiaoli Yan, Zhike Xue, Jincheng Wang, Pengfei Chen, Kaifan Ji, Chun Xia, Liheng Yang, Defang Kong, Zhe Xu, Yian Zhou,…
The Astrophysical Journal  Published: 2025 March 5
DOI:10.3847/1538-4357/adb39e

太陽プロミネンスにおける逆流の起源を解明 (Researchers Uncover Origin of Counterstreaming Flows in Solar Prominences)

Abstract

Solar prominences are very spectacular structures embedded in the tenuous and hot solar corona. Counterstreaming flows, a common feature in solar quiescent prominences, have been discovered for more than 20 yr. However, the mechanism driving the counterstreaming flows is still elusive. To unveil the nature of this phenomenon, we analyzed data of a quiescent prominence observed by the New Vacuum Solar Telescope, the Interface Region Imaging Spectrograph, and the Solar Dynamical Observatory. It is found that there is a distinct longitudinal oscillation of prominence plasma along the higher part of the prominence spine in Hα observations. The oscillation period is approximately 83 minutes and the amplitude is about 32 Mm. The counterstreaming flows are dominant in the middle part of the prominence spine. The velocities of the counterstreaming flows range from about 4 to 11 km s−1. Moreover, intermittent mass flows with upward plumes from the top of the bubbles and tornado-like barbs are observed to be injected into the lower part of the prominence spine from the lower atmosphere. The velocities of these injected mass flows range from about 3 to 30 km s−1. Some injected mass flows exhibit redshifted Doppler signals, while others exhibit blueshifted signals. Based on these high-resolution observations, it is found that different parts of the prominence spine exhibit different dynamic characteristics. These results further advance the understanding of the ubiquitous counterstreaming flows in solar quiescent prominences.

1701物理及び化学
ad
ad
Follow
ad
タイトルとURLをコピーしました