Solar X-ray Monitor On Board the Chandrayaan-2 Orbiter: In-flight Performance and Science Prospects
N. P. S. Mithun, Santosh V. Vadawale, Aveek Sarkar, M. Shanmugam, Arpit R. Patel, Biswajit Mondal, Bhuwan Joshi, Janardhan P., Hiteshkumar L. Adalja, Shiv Kumar… 展开作者
N. P. S. Mithun, Santosh V. Vadawale, Aveek Sarkar, M. Shanmugam, Arpit R. Patel, Biswajit Mondal, Bhuwan Joshi, Janardhan P., Hiteshkumar L. Adalja, Shiv Kumar Goyal, Tinkal Ladiya, Neeraj Kumar Tiwari, Nishant Singh, Sushil Kumar, Manoj K. Tiwari, M. H. Modi, Anil Bhardwaj
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31 pages, 11 figures; accepted for publication in Solar Physics
The Solar X-ray Monitor (abbreviated as XSM) on board India's Chandrayaan-2 mission is designed to carry out broadband spectroscopy of the Sun from lunar orbit. It observes the Sun as a star and measures the spectrum every second in the soft X-ray band of 1 - 15 keV with an energy resolution better than 180 eV at 5.9 keV. The primary objective of the XSM is to provide the incident solar spectrum for the X-ray fluorescence spectroscopy experiment on the Chandrayaan-2 orbiter, which aims to generate elemental abundance maps of the lunar surface. However, observations with the XSM can independently be used to study the Sun as well. The Chandrayaan-2 mission was launched on 22 July 2019, and the XSM began nominal operations, in lunar orbit, from September 2019. The in-flight observations, so far, have shown that its spectral performance has been identical to that on the ground. Measurements of the effective area from ground calibration were found to require some refinement, which has been carried out using solar observations at different incident angles. It also has been shown that the XSM is sensitive enough to detect solar activity well below A-class. This makes the investigations of microflares and the quiet solar corona feasible in addition to the study of the evolution of physical parameters during intense flares. This article presents the in-flight performance and calibration of the XSM instrument and discusses some specific science cases that can be addressed using observations with the XSM.
Elemental Composition Evolution during the 2024 September 30 Solar Eruption: A Comparison of Hot and Cool Plasma Components with Solar Orbiter/SPICE, Hinode/EIS, and Chandrayaan-2/XSM
Southwest Research Institute（西南研究所）；Ann and H.J. Smead Aerospace Engineering Sciences, University of Colorado Boulder（科罗拉多大学博尔德分校安与H.J.斯梅德航空航天工程科学系）；Laboratory for Atmospheric and Space Physics, University of Colorado Boulder（科罗拉多大学博尔德分校大气与空间物理实验室）；University of Alabama in Huntsville（阿拉巴马大学亨茨维尔分校）；NASA Marshall Space Flight Center（美国国家航空航天局马歇尔太空飞行中心）
Observations of the Quiet Sun During the Deepest Solar Minimum of the Past Century with Chandrayaan-2 XSM -- Sub-A Class Microflares Outside Active Regions
Observations of the Quiet Sun During the Deepest Solar Minimum of the Past Century with Chandrayaan-2 XSM -- Elemental Abundances in the Quiescent Corona
A Point-Spread Function for the Extreme Ultraviolet High-Resolution Imager on board Solar Orbiter
Columbia Astrophysics Laboratory, Columbia University（哥伦比亚大学天体物理实验室）；Solar-Terrestrial Centre of Excellence – SIDC, Royal Observatory of Belgium（比利时皇家天文台太阳-地球卓越中心SIDC）；Centre Spatial de Liège, Université de Liège（列日大学空间研究中心）；Max Planck Institute for Solar System Research（马克斯·普朗克太阳系研究所）；Université Paris-Saclay, CNRS, Institut d’Astrophysique Spatiale（巴黎萨克雷大学，法国国家科学研究中心，天体物理研究所）
Cross-Calibration of Chandrayaan-2 XSM with INSPIRESat-1 DAXSS and GOES-16 XRS
Physical Research Laboratory（物理研究实验室）；Space Applications Centre, Indian Space Research Organisation（印度空间研究组织空间应用中心）；Laboratory for Atmospheric and Space Physics, University of Colorado Boulder（科罗拉多大学博尔德分校大气与空间物理实验室）；Space Sciences Laboratory, University of California Berkeley（加州大学伯克利分校空间科学实验室）；Southwest Research Institute（西南研究所）；Cooperative Institute for Research in Environmental Sciences, University of Colorado Boulder（科罗拉多大学博尔德分校环境科学研究合作学院）；NOAA National Centers for Environmental Information（美国国家海洋和大气管理局国家环境信息中心）
Fast and periodic propagating disturbances along coronal loops detected with EUI on board Solar Orbiter
Max Planck Institute for Solar System Research（马克斯·普朗克太阳系研究所）；Physikalisch-Meteorologisches Observatorium Davos, World Radiation Center（达沃斯物理气象观测站，世界辐射中心）；Centre for mathematical Plasma Astrophysics, Mathematics Department, KU Leuven（鲁汶大学数学系等离子体天体物理学中心）；Solar-Terrestrial Centre of Excellence – SIDC, Royal Observatory of Belgium（比利时皇家天文台太阳-地球卓越中心-SIDC）；LPC2E, OSUC, Univ Orleans, CNRS, CNES（奥尔良大学空间环境与条件研究中心（LPC2E））；School of Engineering, Physics, and Mathematics, Northumbria University（诺森比亚大学工程、物理与数学学院）；European Space Agency (ESA), European Space Research and Technology Centre (ESTEC)（欧洲航天局（ESA）欧洲空间研究与技术中心（ESTEC））；ETH-Zürich（苏黎世联邦理工学院）
Moving structures in ultraviolet bright points: observations from Solar Orbiter/EUI
在活动区域的日冕亮点和太阳耀斑中检测到了移动结构，它们是双向的，对称的，同时的和准周期的（Ning & Guo 2014; Ning 2016; Li et al. 2016 a）。它们可以被视为等离子体通过磁重联流出的观测证据。在这篇文章中，我们探索了2020年11月19日在安静的太阳或一个小的活动区域内观察到的15个紫外亮点（UBP）中的成对移动结构，并由太阳轨道器（SolO）上的极紫外成像仪（EUI）的高分辨率（HRI）望远镜在两个通带HRIEUV 174和HRILyα 1216中测量。在10个UBP中观测到的运动结构从亮核开始向两端传播，解释为双向运动结构的发散运动。这些移动结构的特点也是对称性和对称性，在七个UBP的情况下，他们表现出准周期性。它们可能是由磁重联后的流出产生的。另外5个UBP中的运动结构起源于双端，并逐渐靠近，合并在一起，表现为会聚运动，这可能是由通过磁重联的流入引起的，也可能被解释为色球蒸发驱动的上升流。
Propagating brightenings in small loop-like structures in the quiet Sun corona: Observations from Solar Orbiter/EUI
在太阳极紫外（EUV）图像中观察到的增亮通常被解释为在过渡区或日冕温度下发生的微米或纳米耀斑的特征。太阳轨道飞行器上的极紫外线成像仪（EUI）最近的观测显示，在安静的太阳日冕中，这种亮度（称为篝火）最小。从2020年5月30日开始，以约400 km的分辨率分析太阳上的EUI 174数据，节奏为5 s，我们在这里报告了一些情况，这些篝火沿着其明显的小（3-5 Mm）环状结构表现出传播特征。测量的传播速度通常在25 km s $^{-1}$和60 km s $^{-1}$之间。如果假设环形等离子体的温度为一百万开尔文，那么这些视在的运动将比局部声速慢。此外，这些增亮表现出非平凡的传播特性，如分叉，合并，反射和重复等离子体喷射。我们认为，这些功能是这些小尺度的磁结构的内部动力学的表现，并可以提供重要的见解的动态响应（$\sim$ 40秒）的环路等离子体的加热事件，以及到加热事件本身的位置。
Connecting Solar Orbiter remote-sensing observations and Parker Solar Probe in-situ measurements with a numerical MHD reconstruction of the Parker spiral
