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The solar wind plasma upstream of Mars observed by Tianwen-1:Comparison with Mars Express and MAVEN

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Science China Earth Sciences 2022年第4期65卷 759-768页

作者： Kai FAN Limei YAN Yong WEI Aibing ZHANG Linggao KONG Markus FRÄNZ Fei HE Lihui CHAI Chongjing YUAN Yuqi WANG Jun ZHONG Zhaojin RONG Zhonghua YAO Yongxin PAN Jun CUI Jiansen HE Wenya LI Binbin TANG Chi WANG Key Laboratory of Earth and Planetary Physics Institute of Geology and GeophysicsChinese Academy of SciencesBeijing 100029China College of Earth and Planetary Sciences University of Chinese Academy of SciencesBeijing 100049China National Space Science Center Chinese Academy of SciencesBeijing 100190China Beijing Key Laboratory of Space Environment Exploration Beijing 100190China Key Laboratory of Science and Technology on Space Environment Situational Awareness Chinese Academy of SciencesBeijing 100190China Max-Planck-Institute for solar System Research Goettingen 37077Germany State Key Laboratory of Space Weather Chinese Academy of SciencesBeijing 100190China School of Atmospheric Sciences Sun Yat-Sen UniversityZhuhai 519082China Institute of Space Physics and Applied Technology Peking UniversityBeijing 100871China

On the great journey to Mars,China’s first planetary exploration mission,the Tianwen-1 came within 26 million kilometers of Mars from 31 October 2020 to 25 January 2021 and was getting closer to its destination,the red planet,in search of answers to the cataclysmic climate change that occurred in Martian *** the escape of the Martian atmosphere and the loss of surface water were firmly influenced by solar ***-1 provided a unique chance to depict the solar wind streams between Earth and Mars during the minimum of solar Cycle *** the three-month cruise phase of Tianwen-1,the solar wind flows were successively observed at Earth,Tianwen-1,and *** the field of view correction and noise reduction,the solar wind velocity and density measured by Tianwen-1 show good agreement with those at Earth and *** results indicate that the performance of the ion analyzer onboard the Tianwen-1 orbiter is reliable and *** is worth looking forward to the joint observations of ion escape with other Mars probes in the following Martian years.

关键词： Tianwen-1 Mars Plasma moment solar wind

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Magnetohydrodynamics (MHD) numerical simulations on the interaction of the solar wind with the magnetosphere: A review

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Science China Earth Sciences 2013年第7期56卷 1141-1157页

作者： WANG Chi GUO XiaoCheng PENG Zhong TANG BinBin SUN TianRan LI WenYa HU YouQiu State Key Laboratory of Space Weather Center for Space Science and Applied Research Chinese Academy of Sciences School of Earth and Space Sciences University of Science and Technology of China

The magnetosphere is the outermost layer of the geospace, and the interaction of the solar wind with the magnetosphere is the key element of the space weather cause-and-effect chain process from the Sun to Earth, which is one of the most challenging scientific problems in the geospace weather study. The nonlinearity, multiple component, and time-dependent nature of the geospace make it very difficult to describe the physical process in geospace using traditional analytic analysis approach. Numerical simulations, a new research tool developed in recent decades, have a deep impact on the theory and application of the geospace. MHD simulations started at the end of the 1970s, and the initial study was limited to two-dimensional (2D) cases. Due to the intrinsic three-dimensional (3D) characteristics of the geospace, 3D MHD simulations emerged in the 1980s, in an attempt to model the large-scale structures and fundamental physical processes in the magnetosphere. They started to combine with the space exploration missions in the 1990s and make comparisons with observations. Physics-based space weather forecast models started to be developed in the 21st century. Currently only a few space-power countries such as USA and Japan have developed 3D magnetospheric MHD models. With the rapid advance of space science in China, we have developed a new global MHD model, namely PPMLR-MHD, which has high order spatial accuracy and low numerical dissipation. In this review, we will briefly introduce the global 3D MHD modeling, especially the PPMLR-MHD code, and summarize our recent work based on the PPMLR-MHD model, with an emphasis on the interaction of interplanetary shocks with the magnetosphere, large-scale current systems, reconnection voltage and transpolar potential drop, and Kelvin-Helmholtz (K-H) instability at the magnetopause.

关键词： solar wind magnetosphere MHD simulations

Effect of solar wind plasma parameters on space weather

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Research in Astronomy and Astrophysics 2015年第1期15卷 85-106页

作者： Balveer S.Rathore Dinesh C.Gupta Subhash C.Kaushik School of Study in Physics Jiwaji UniversityGwalior Madhya Pradesh India

Today’s challenge for space weather research is to quantitatively predict the dynamics of the magnetosphere from measured solar wind and interplanetary magnetic field（IMF） conditions. Correlative studies between geomagnetic storms（GMSs）and the various interplanetary（IP） field/plasma parameters have been performed to search for the causes of geomagnetic activity and develop models for predicting the occurrence of GMSs, which are important for space weather predictions. We find a possible relation between GMSs and solar wind and IMF parameters in three different situations and also derived the linear relation for all parameters in three *** the basis of the present statistical study, we develop an empirical model. With the help of this model, we can predict all categories of GMSs. This model is based on the following fact： the total IMF Btotalcan be used to trigger an alarm for GMSs, when sudden changes in total magnetic field Btotaloccur. This is the first alarm condition for a storm’s arrival. It is observed in the present study that the southward Bzcomponent of the IMF is an important factor for describing GMSs. A result of the paper is that the magnitude of Bzis maximum neither during the initial phase（at the instant of the IP shock） nor during the main phase（at the instant of Disturbance storm time（Dst） minimum）. It is seen in this study that there is a time delay between the maximum value of southward Bzand the Dst minimum, and this time delay can be used in the prediction of the intensity of a magnetic storm two-three hours before the main phase of a GMS. A linear relation has been derived between the maximum value of the southward component of Bzand the Dst, which is Dst =（-0.06）＋（7.65）Bz＋ *** auxiliary conditions should be fulfilled with this, for example the speed of the solar wind should, on average, be 350 km s-1 to 750 km s-1, plasma β should be low and, most importantly, plasma temperature should be low for intense storms. If the plasma tem

关键词： solar wind geomagnetic storms(GMSs) interplanetary magnetic field(IMF)

Propagation of large-scale solar wind events in the outer heliosphere from a numerical MHD simulation

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Earth and Planetary Physics 2021年第3期5卷 223-231页

作者： XiaoCheng Guo YuCheng Zhou Chi Wang Ying DLiu State Key Laboratory of Space Weather National Space Science CenterChinese Academy of ScienceBeijing 100190China College of Earth and Planetary Sciences University of Chinese Academy of SciencesChinese Academy of ScienceBeijing 100049China

Voyager 1 occasionally detected sudden jumps of the local interstellar magnetic field strength since its heliopause crossing in August *** events were believed to be associated with outward propagating solar wind shocks originating in the inner *** we investigate the correlation between interstellar shocks and large-scale solar wind events by means of numerical MHD *** solar wind is simplified as a symmetric flow near the equatorial plane,and the interstellar neutrals are treated as a constant flow with a fixed density distribution along the upwind direction of the local interstellar *** charge exchanges between the solar wind plasma and the interstellar neutrals are taken into *** a heliocentric distance of 1 AU,the solar wind data from OMNI,STEREO A and B during the period between 2010 and 2017 are used as the inner boundary conditions to drive the *** simulation results showed that the solar wind gradually merges into large-scale structures as the radial distance increases,consistent with observations by New *** propagating into the inner heliosheath,the shocks are fully developed and the corresponding pressure pulses roughly agree with the observations by Voyager 2 in the inner *** arrival of the shocks beyond the heliopause is estimated and found to be consistent with the observed signatures of interstellar shocks by Voyager *** possible origins of interstellar shocks in the inner heliosheath are discussed based on the simulation.

关键词： MHD outer heliosphere solar wind interstellar medium shocks Voyager

Tianwen-1 MINPA observations in the solar wind

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Earth and Planetary Physics 2022年第1期6卷 1-9页

作者： AiBing Zhang LingGao Kong WenYa Li Lei Li BinBin Tang ZhaoJin Rong Yong Wei JiJie Ma YiTeng Zhang LiangHai Xie YuXian Wang JianSen He Bin Liu WenJing Wang Bin Su JiaWei Li Xu Tan Fang Wang TaiFeng Jin FuHao Qiao Peter Wurz Yan Zhu YunFei Bai YiRen Li XinBo Zhu YueQiang Sun YongLiao Zou Chi Wang National Space Science Center Chinese Academy of SciencesBeijing 100190China Beijing Key Laboratory of Space Environment Exploration Beijing 100190China Key Laboratory of Science and Technology on Space Environment Situational Awareness Chinese Academy of SciencesBeijing 100190China University of Chinese Academy of Sciences Beijing 100049China State Key Laboratory of Space Weather Chinese Academy of SciencesBeijing 100190China Key Laboratory of Earth and Planetary Physics Institute of Geology and GeophysicsChinese Academy of SciencesBeijing 100029China Institute of Space Physics and Applied Technology Peking UniversityBeijing 100871China Lunar Exploration and Space Engineering Center Beijing 100190China National Astronomical Observatories Chinese Academy of SciencesBeijing 100012China Physics Institute University of BernBern 3012Switzerland University of Science and Technology of China Hefei 230026China Shanghai Academy of Spaceflight Technology Shanghai 201109China

The Mars Ion and Neutral Particle Analyzer(MINPA)is one of the three scientific instruments onboard the Tianwen-1 orbiter to investigate the Martian space *** Tianwen-1’s transfer orbit to Mars,the MINPA was switched on to measure the solar wind ***,we present the first results of the MINPA observations in the solar *** cruise,nearly half of the MINPA ion field-of-view(FOV)was blocked by the lander capsule;thus only the solar-wind ions with azimuthal speeds pointing towards the unblocked FOV sectors could be *** perform a detailed comparison of the MINPA’s solar wind observations with data from Earth-based missions when MINPA reached its count-rate peak,finding a general consistency of the ion moments between *** blocking effect due to the lander is evaluated quantitatively under varying solar-wind velocity *** the blocking effect,the MINPA’s solar wind measurements during the transfer orbit suggest a good performance.

关键词： MINPA Tianwen-1 solar wind capsule blocking effect

Validation of the use of THEMIS-B and THEMIS-C as a near-Earth solar wind monitor

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Earth and Planetary Physics 2022年第6期6卷 546-554页

作者： DianJun Zhang WenLong Liu Zhao Zhang School of Space and Environment Beihang UniversityBeijing 100191China Key Laboratory of Space Environment Monitoring and Information Processing Ministry of Industry and Information TechnologyBeijing 100191China

Two THEMIS(Time History of Events and Macroscale Interactions during Substorms)spacecraft,B and C,began orbiting the Moon in 2011 and have since provided routine measurements of the plasma conditions in the lunar *** this study,we systematically compare these measurements in near-Earth space with solar wind measurements obtained from the Lagrangian 1(L1)point and propagated to the Earth,including measurements in the OMNI database and from the wind spacecraft.A statistical comparison between THEMIS data and data from the OMNI database from September 2011 to December 2017 showed that the Y and Z components of the magnetic field and the flow speed are generally consistent between the two data *** ion number density and the dynamic pressure measured by THEMIS in near-Earth space are lower than those in the OMNI database,suggesting possible variation in the solar wind environment while propagating from the L1 point to near-Earth *** further show two examples in which near-Earth solar wind measurements are applied in calculating the magnetopause location and in quantifying the magnetic field response to interplanetary *** examples suggest that using solar wind data from near-Earth space achieves better results than using solar wind data from the L1 *** results provide validation of THEMIS-B and THEMIS-C as an alternative monitor of the near-Earth solar wind environment.

关键词： interplanetary shocks solar wind magnetosphere

Is solar wind electron precipitation a source of neutral heating in the nightside Martian upper atmosphere?

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Earth and Planetary Physics 2021年第1期5卷 1-10页

作者： LongKang Dai Jun Cui DanDan Niu Hao Gu YuTian Cao XiaoShu Wu HaiRong Lai Planetary Environmental and Astrobiological Research Laboratory(PEARL) School of Atmospheric SciencesSun Yat-sen UniversityZhuhai Guangdong 519082China Key Laboratory of Lunar and Deep Space Exploration National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China Center for Excellence in Comparative Planetology Chinese Academy of SciencesHefei 230031China Institute of Space Science and Applied Technology Harbin Institute of TechnologyShenzhen Guangdong 518055China

solar wind(SW)electron precipitation is able to deposit a substantial amount of energy in the nightside Martian upper atmosphere,potentially exerting an influence on its thermal *** study serves as the first investigation of such an issue,with the aid of the simultaneous measurements of both neutral density and energetic electron intensity made on board the recent Mars Atmosphere and Volatile Evolution(MAVEN)*** report that,from a statistical point of view,the existing measurements do not support a scenario of noticeable neutral heating via SW electron ***,during 3%−4%of the MAVEN orbits for which data are available,strong correlation between nightside temperature and electron intensity is observed,manifested as collocated enhancements in both parameters,as compared to the surrounding *** addition,our analysis also indicates that neutral heating via SW electron precipitation tends to be more effective at altitudes below 160 km for integrated electron intensities above 0.01 ergs·cm^−2·s^−1 over the energy range of 3−450 *** results reported here highlight the necessity of incorporating SW electron precipitation as a heat source in the nightside Martian upper atmosphere under extreme circumstances such as during interplanetary coronal mass ejections.

关键词： Mars solar wind upper atmosphere MAVEN

Acceleration of solar wind particles due to inertial Alfvén waves

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Communications in Theoretical Physics 2024年第6期76卷 137-141页

作者： Kiran Batool Imran A Khan M Shamir Abdul Kabir S Ayaz Theoretical Physics Department National Centre for PhysicsIslamabad 44000Pakistan Department of Space Sciences Institute of Space TechnologyIslamabad 44000Pakistan Space and Astrophysics Research Lab(SARL) National Center of GIS and Space Applications(NCGSA)Islamabad 44000Pakistan Salam Chair Department of PhysicsGC University LahoreKatchery RoadLahorePunjab 54000Pakistan Department of Space Science and CSPAR University of Alabama in HuntsvilleHuntsvilleAL 35899United States of America

Gaining an understanding of the effects and dynamics of the solar wind is crucial for the study of space weather,Earth's magnetosphere,spacecraft protection,the dynamics of the solar System,and various other *** show that Alfvén waves effectively transfer energy to resonant *** study demonstrates how inertial Alfvén waves deliver their energy to resonant plasma particles in different solar environments under certain *** analysis shows that inertial Alfvén waves experience more rapid damping with increasing parallel wavenumber,ambient magnetic field strength,and particle number density,coupled with a decrease in *** rate of energy transfer to resonant particles intensifies with higher temperatures and reduced parallel wavenumber and particle number *** with higher initial velocities actively participate in Landau damping,especially in regions with a stronger ambient magnetic field.

关键词： solar wind inertial Alfven waves resonant particles

Single-Fluid 2D Magnetohydrodynamic Simulation of solar wind Structure in Comparison to Ulysses Observations

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Wuhan University Journal of Natural Sciences 2000年第4期5卷 447-450页

作者： Deng Ling-yun, Wang Jing-fang, Xiang Chang-qing, Xiong Dong-hui College of Electronic Information, Wuhan University, Wuhan 430072, China College of Electronic Information Wuhan University Wuhan China

Two dimensional Magnetohydrodynamic (MHD) equations with and without the momentum addition respectively have been used to simulate the solar wind structure on the meridian plane. The results show that far away from the sun it isn't solar magnetic field that induces the cncave solar wind speed. Instead, there may be the fast speed streamer driven by the momentum addition and an interface between high and low speed streamers. The interaction between high and low speed streamers causes the sharp division.

关键词： solar wind solar magnetic momentum addition