A Space Weather Mission Concept: Observatories of the Solar Corona and Active Regions (OSCAR)
Antoine Strugarek, Nils Janitzek, Arrow Lee, Philipp Löschl, Bernhard Seifert, Sanni Hoilijoki, Emil Kraaikamp, Alankrita Isha Mrigakshi, Thomas Philippe, Sheil… 展开作者
Antoine Strugarek, Nils Janitzek, Arrow Lee, Philipp Löschl, Bernhard Seifert, Sanni Hoilijoki, Emil Kraaikamp, Alankrita Isha Mrigakshi, Thomas Philippe, Sheila Spina, Malte Bröse, Sonny Massahi, Liam O'Halloran, Victor Pereira Blanco, Christoffer Stausland, Philippe Escoubet, Günter Kargl
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28 pages, 7 figures, 6 tables, accepted for publication in Space Weather and Space Climate
Coronal Mass Ejections (CMEs) and Corotating Interaction Regions (CIRs) are major sources of magnetic storms on Earth and are therefore considered to be the most dangerous space weather events. The Observatories of Solar Corona and Active Regions (OSCAR) mission is designed to identify the 3D structure of coronal loops and to study the trigger mechanisms of CMEs in solar Active Regions (ARs) as well as their evolution and propagation processes in the inner heliosphere. It also aims to provide monitoring and forecasting of geo-effective CMEs and CIRs. OSCAR would contribute to significant advancements in the field of solar physics, improvements of the current CME prediction models, and provide data for reliable space weather forecasting. These objectives are achieved by utilising two spacecraft with identical instrumentation, located at a heliocentric orbital distance of 1~AU from the Sun. The spacecraft will be separated by an angle of 68$^{\circ}$ to provide optimum stereoscopic view of the solar corona. We study the feasibility of such a mission and propose a preliminary design for OSCAR.
The First Scientific Flight and Observations of the 50-mm Balloon-Borne White-Light Coronagraph
Yunnan Observatories, Chinese Academy of Sciences（中国科学院云南天文台）；Yunnan Key Laboratory of the Solar physics and Space Science（云南省太阳物理与空间科学重点实验室）；Aerospace Information Research Institute, Chinese Academy of Sciences（中国科学院空天信息创新研究院）；University of Chinese Academy of Sciences（中国科学院大学）；Center for Astronomical Mega-Science, Chinese Academy of Sciences（中国科学院国家天文台）；Institute of Space Sciences, Shandong University（山东大学空间科学研究院）；Kunming University of Science and Technology（昆明理工大学）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；Southwest Jiaotong University（西南交通大学）
Spectroscopic He I 1083 nm prominence eruption observations in the middle corona with MLSO/UCoMP
Taylor University（泰勒大学）；Southwest Research Institute（西南研究所）；High Altitude Observatory, NSF National Center for Atmospheric Research（高山观测站，美国国家科学基金会国家大气研究中心）
利用MLSO/UCoMP在He I 1083 nm观测中探测日珥喷射，提供动态行为信息以改进空间天气预报。
The detection of upwardly propagating waves channelling energy from the chromosphere to the low corona
几十年来，人们对太阳大气中的波动运动进行了普遍的观测。最近对空间和地面观测站的改进使重点转向太阳表面较小的磁结构。在本文中，高分辨率的地面数据，使用瑞典1米太阳望远镜的空间和时间的数据相结合的大气成像组件（AIA）的太阳动力学观测（SDO）卫星上分析运行半影波（RPWs）。RPW一直被认为是发生在太阳黑子内的径向波传播。最近的研究表明，它们实际上是向上传播的场向波（UPWs）。在这里，RPWs在太阳能孔内首次被观察到，并被解释为UPWs由于缺乏半影，需要支持RPWs。这些UPW也被观察到co-spatially和co-temporarily内的几个SDO/AIA元素线，采样的过渡区和低电晕。观测到的UPW的水平速度约为17 +-0.5 km s-1，最小垂直速度为42 +-21 km s-1。波的估计能量约为150 W m-2，这是加热安静的太阳日冕所需的下限。这是太阳色球层和低日冕中一种新的、尚未被考虑的波能来源。
Diagnosing the magnetic field structure of a coronal cavity observed during the 2017 total solar eclipse
我们在2017年8月21日的日全食期间，使用北京大学的望远镜在日冕红线Fe X 6374和使用中国科学院云南天文台的望远镜在绿线Fe XIV 5303的西边缘上方观测到日冕空洞。利用太阳动力学观测站（SDO）上的日震磁成像仪在日食前一周拍摄的地磁图，建立了一系列的磁场模型。然后将模型场线与SDO上的大气成像组件拍摄的图像和我们的日冕红线图像中看到的日冕结构进行比较。最佳拟合模型由扭角为3.1 $π$的通量绳组成，这与在1天文单位观测到的行星际通量绳总扭角的最可能值一致。根据这个模型计算的Fe XIII 10747的线偏振显示了一个“lagomorphic”的特征，这也被高海拔天文台的日冕多通道偏振仪观测到。我们还发现，在Fe XIII 10747的视线速度的环形结构，这意味着热等离子体沿螺旋磁场结构，在腔中。这些结果表明，空腔的磁结构是一个高度扭曲的磁通绳，最终可能爆发。利用Fe XIII 10747 γ和Fe X 6374 γ的强度比研究了腔的温度结构。
Simulating the photospheric to coronal plasma using magnetohydrodynamic characteristics III: validation including gravity, flux emergence, and an eruption
National Solar Observatory（国家太阳观测台）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；U.S. Naval Research Laboratory（美国海军研究实验室）
Unprecedented Multipoint Observation of Spatially Varying ICME Turbulence of Different Ages during October 2024 Extreme Solar Storm at 1 AU
Space Physics Laboratory, Vikram Sarabhai Space Centre, Indian Space Research Organization（印度空间研究组织维克拉姆萨拉巴伊航天中心空间物理实验室）；Department of Physics, University of Kerala（喀拉拉大学物理系）；National Institute for Astrophysics, Institute for Space Astrophysics and Planetology（意大利国家天体物理研究所空间天体物理学与行星科学研究所）；Centre for Space Science and Technology, Indian Institute of Technology Roorkee（印度鲁尔凯理工学院空间科学与技术中心）；Physical Research Laboratory（物理研究实验室）
