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arXiv 2025年

作者： Srivastava, A.K. Mondal, Sripan Priest, Eric R. Mishra, Sudheer K. Pontin, David I. Kwon, R.Y. Yuan, Ding Murawski, K. Asai, Ayumi Varanasi221005 India Mathematics Institute St Andrews University St AndrewsKY16 9SS United Kingdom Astronomical Observatory Kyoto University Sakyo Kyoto606-8502 Japan School of Information and Physical Sciences University of Newcastle Australia Korea Astronomy and Space Science Institute Daejeon34055 Korea Republic of Shenzhen Key Laboratory of Numerical Prediction for Space Storm Institute of Space Science and Applied Technology Harbin Institute of Technology Guangdong Shenzhen China Institute of Physics University of Maria Curie-Sklodowska Pl. M. Curie-Sklodowskiej 5 Lublin20-031 Poland

The Sun’s outer atmosphere, the corona, is maintained at mega-Kelvin temperatures and fills the heliosphere with a supersonic outflowing wind. The dissipation of magnetic waves and direct electric currents are likely to be the most significant processes for heating the corona, but a lively debate exists on their relative roles. Here, we suggest that the two are often intrinsically linked, since magnetic waves may trigger current dissipation, and impulsive reconnection can launch magnetic waves. We present a study of the first of these processes by using a 2D physics-based numerical simulation using the Adaptive Mesh Refined (AMR) Versatile Advection Code (VAC). Magnetic waves such as fast magnetoacoustic waves are often observed to propagate in the large-scale corona and interact with local magnetic structures. The present numerical simulations show how the propagation of magnetic disturbances towards a null point or separator can lead to the accumulation of the electric currents. Lorentz forces can laterally push and vertically stretch the magnetic fields, forming a current sheet with a strong magnetic-field gradient. The magnetic field lines then break and reconnect, and so contribute towards coronal heating. Numerical results are presented that support these ideas and support the concept of a symbiosis between waves and reconnection in heating the solar corona. Copyright © 2025, The Authors. All rights reserved.

关键词： Lorentz force

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Effects of Martian crustal magnetic field on its ionosphere

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Science China(Technological Sciences) 2010年第6期53卷 1717-1724页

作者： ZOU Hong,CHEN HongFei,YU Ning,SHI WeiHong,YU XiangQian,ZOU JiQing & ZHONG WeiYing institute of space physics and applied technology,Peking University,Beijing 100871,China Institute of Space Physics and Applied Technology Peking University Beijing China

The effect of the Martian crustal magnetic field is one of the hot topics of the study of Martian *** studies on this topic are summarized in this *** data of the Martian ionosphere were resulted from radio occultation *** to the observations,the electron density scale height and the peak electron density of the Martian ionosphere are influenced by its crustal magnetic *** strong horizontal magnetic field prevents the vertical diffusion of the plasma and makes the electron density scale height in the topside ionosphere close to that in the photo equilibrium *** the cusp-like regions with strong vertical magnetic field,the enhanced vertical diffusion leads to a larger electron density scale height in the diffusion equilibrium *** observation of radio occultation experiment onboard Mars Global Surveyor (MGS) showed that the averaged peak electron density observed in the southern hemisphere with strong crustal magnetic field was slightly larger than that in the northern hemisphere with weak crustal magnetic *** Mars advanced radar for subsurface and ionosphere sounding (MARSIS) onboard Mars Express (MEX) was the first topside sounder to be used to observe Martian *** MARSIS results confirmed that the enhancement of the peak electron density occurred in cusp-like regions with open field lines,and the amount of the enhancement was much larger than that observed by the radio occultation *** are two possible mechanisms for the peak electron density enhancement in the cusp-like crustal magnetic field regions:One is the precipitation of the energetic particles and the other is the heating by the waves excited by plasma ***'s difficult to determine which one is the key mechanism for the peak electron density *** on these studies,several interesting problems on the Martian ionosphere and plasma environment are presented.

关键词： Mars exploration Martian crustal megnetic field Martian ionosphere energetic particles detection plasma wave detection

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Analysis of the internal charging data in medium earth orbit with numerical simulation and ground experiment

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Science China(Technological Sciences) 2022年第4期65卷 977-986页

作者： SONG SiYu CHEN HongFei YU XiangQian ZOU Hong ZONG QiuGang CHEN Ao SHI WeiHong YE YuGuang Institute of Space Physics and Applied Technology School of Earth and Space SciencesPeking UniversityBeijing 100871China

The deep dielectric charging effect monitor(DDCEM)has been designed to study the internal charging effect by measuring the charging currents and potentials inside the *** is equipped on three Chinese navigation satellites in a circular medium earth orbit(MEO)with 22000 km average height and 55°*** simulation based on the Geant4-RIC method was used to evaluate the data of *** data during May to November 2019 on one of the three satellites show that the charging currents of DDCEM were negatively enhanced when the satellite moved into the outer radiation *** currents reached the negative maximum during a significant electron enhancement in September *** currents were also detected besides negative currents that were caused by the deposition of electrons in the *** causation of positive currents in the space environment may be that the low-energy electrons cannot penetrate the satellite skin and make it charging to negative potential,the reference ground of DDCEM that is connected to the satellite skin drops below zero by the low-energy electrons so that the output currents turn to *** experiment was used to simulate the causation of positive currents and the result verified our theory.

关键词： deep dielectric charging effect monitor internal charging effect charging currents and potentials medium earth orbit space environment

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The PLATO mission

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Experimental Astronomy 2025年第3期59卷 1-111页

作者： Rauer, Heike Aerts, Conny Cabrera, Juan Deleuil, Magali Erikson, Anders Gizon, Laurent Goupil, Mariejo Heras, Ana Walloschek, Thomas Lorenzo-Alvarez, Jose Marliani, Filippo Martin-Garcia, César Mas-Hesse, J. Miguel O’Rourke, Laurence Osborn, Hugh Pagano, Isabella Piotto, Giampaolo Pollacco, Don Ragazzoni, Roberto Ramsay, Gavin Udry, Stéphane Appourchaux, Thierry Benz, Willy Brandeker, Alexis Güdel, Manuel Janot-Pacheco, Eduardo Kabath, Petr Kjeldsen, Hans Min, Michiel Santos, Nuno Smith, Alexis Suarez, Juan-Carlos Werner, Stephanie C. Aboudan, Alessio Abreu, Manuel Acuña, Lorena Adams, Moritz Adibekyan, Vardan Affer, Laura Agneray, François Agnor, Craig Aguirre Børsen-Koch, Victor Ahmed, Saad Aigrain, Suzanne Al-Bahlawan, Ashraf Alcacera Gil, Ma de los Angeles Alei, Eleonora Alencar, Silvia Alexander, Richard Alfonso-Garzón, Julia Alibert, Yann Allende Prieto, Carlos Almeida, Leonardo Alonso Sobrino, Roi Altavilla, Giuseppe Althaus, Christian Alvarez Trujillo, Luis Alonso Amarsi, Anish Ammler-von Eiff, Matthias Amôres, Eduardo Andrade, Laerte Antoniadis-Karnavas, Alexandros António, Carlos Aparicio del Moral, Beatriz Appolloni, Matteo Arena, Claudio Armstrong, David Aroca Aliaga, Jose Asplund, Martin Audenaert, Jeroen Auricchio, Natalia Avelino, Pedro Baeke, Ann Baillié, Kevin Balado, Ana Ballber Balagueró, Pau Balestra, Andrea Ball, Warrick Ballans, Herve Ballot, Jerome Barban, Caroline Barbary, Gaële Barbieri, Mauro Barceló Forteza, Sebastià Barker, Adrian Barklem, Paul Barnes, Sydney Barrado Navascues, David Barragan, Oscar Baruteau, Clément Basu, Sarbani Baudin, Frederic Baumeister, Philipp Bayliss, Daniel Bazot, Michael Beck, Paul G. Belkacem, Kevin Bellinger, Earl Benatti, Serena Benomar, Othman Bérard, Diane Bergemann, Maria Bergomi, Maria Bernardo, Pierre Biazzo, Katia Bignamini, Andrea Bigot, Lionel Billot, Nicolas Binet, Martin Biondi, David Biondi, Federico Birch, Aaron C. Bitsch, Bertram Bluhm Ceballos, Paz Victoria Bódi, Attila Bognár, Zsófia Boisse, Isabelle Bolmont, Emeline Bonanno, Alfio Bonavita, Institut für Planetenforschung Deutsches Zentrum für Luft- und Raumfahrt DLR Rutherfordstrasse 2 Berlin 12489 Germany Fachbereich Geowissenschaften Institut für Geologische Freie Universität Berlin Malteserstr. 74-100 Berlin 12249 Germany Institute of Astronomy KU Leuven Leuven Belgium CNRS CNES LAM Aix Marseille University Marseille France Max Planck Institute for Solar System Research Göttingen Germany LESIA Paris Observatory PSL University Sorbonne University Paris Cité University CNRS Meudon France ESTEC European Space Agency Noordwijk Netherlands ESAC European Space Agency Madrid Spain Centro de Astrobiología CSIC-INTA Campus ESAC Madrid Spain Center for Space and Habitability University of Bern Bern Switzerland INAF - Osservatorio Astrofisico di Catania Catania Italy Department of Physics and Astronomy University of Padua Padua Italy Department of Physics University of Warwick Coventry United Kingdom Astronomical Observatory of Padova INAF - Italian National Institute for Astrophysics Padua Italy Armagh Observatory and Planetarium College Hill Armagh United Kingdom Geneve Observatory University of Geneve Geneve Switzerland IAS University of Paris-Saclay Orsay France AlbaNove University Centre Stockholm University Stockholm Sweden Department of Astrophysics University of Vienna Vienna Austria Department of Astronomy University of Sao Paulo Sao Paulo Brazil Astronomical Institute of the Czech Academy of Sciences Ondřejov Czech Republic Department of Physics and Astronomy Aarhus University Aarhus Denmark Institute for Space Research SRON Leiden Netherlands Instituto de Astrofísica e Ciências do Espaço CAUP Universidade do Porto Porto Portugal Departamento de Física e Astronomia Faculdade da Ci ncias Universidade do Porto Porto Portugal Mullard Space Science Laboratory University College London Holmbury Saint Mary United Kingdom Dept. Theoretical Physics and the Cosmos University of Granada Granada Spain Centre for Plan

PLATO (PLAnetary Transits and Oscillations of stars) is ESA’s M3 mission designed to detect and characterise extrasolar planets and perform asteroseismic monitoring of a large number of stars. PLATO will detect small planets (down to <2REarth) around bright stars (<11 mag), including terrestrial planets in the habitable zone of solar-like stars. With the complement of radial velocity observations from the ground, planets will be characterised for their radius, mass, and age with high accuracy (5%, 10%, 10% for an Earth-Sun combination respectively). PLATO will provide us with a large-scale catalogue of well-characterised small planets up to intermediate orbital periods, relevant for a meaningful comparison to planet formation theories and to better understand planet evolution. It will make possible comparative exoplanetology to place our Solar System planets in a broader context. In parallel, PLATO will study (host) stars using asteroseismology, allowing us to determine the stellar properties with high accuracy, substantially enhancing our knowledge of stellar structure and evolution. The payload instrument consists of 26 cameras with 12cm aperture each. For at least four years, the mission will perform high-precision photometric measurements. Here we review the science objectives, present PLATO‘s target samples and fields, provide an overview of expected core science performance as well as a description of the instrument and the mission profile towards the end of the serial production of the flight cameras. PLATO is scheduled for a launch date end 2026. This overview therefore provides a summary of the mission to the community in preparation of the upcoming operational phases. © The Author(s) 2025.

关键词： Asteroseismology Exoplanets PLATO mission

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Dependence of Secondary Ion Mass Spectrometry Relative Sensitivity Factor on Matrix

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Chinese physics Letters 1998年第9期15卷 697-699页

作者： YANG De-quan FAN Chui-zhen Laboratory of Applied Surface Physics Lanzhou Institute of PhysicsChinese Academy of Space TechnologyLanzhou 730000

In secondary ion mass spectrometry,we define the slope of logarithm of relative sensitivity factor versus ionization potential as matrix effect *** was found that the matrix effect factor is dependent on the average atomic number and average electronegative values,as well as average oxide formation heat of ***"combined local thermal equilibrium model and bond-breaking" model proposed by us early was used to explain this dependence.

关键词： breaking logarithm equilibrium

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Explaining the dynamics of the sub-relativistic electron third belt in the Earth's radiation belts by using medium Earth orbit satellite observations

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Earth and Planetary physics 2024年第5期8卷 762-775页

作者： JiaLi Chen Hong Zou YuGuang Ye Institute of Space Physics and Applied Technology Peking UniversityBeijing 100871China

The Earth's electron radiation belts typically exhibit a two-belt ***,observations from the Van Allen Probes revealed the existence of a three-belt *** structure consists of an inner belt,a slot region,a remnant belt,a“second slot,”and a new outer belt(or the“third belt”).The formation of the structure involves both the partial loss of the original outer belts and the formation of the third *** processes are likely associated with radial diffusion induced by ultra-low-frequency(ULF)*** this study,we mainly analyzed electron flux data from medium Earth orbit(MEO)navigation satellites M17–M19 to supplement the observational evidence for the sub-relativistic electron(~100–500 keV)three-belt *** of substorm injections and ULF waves during the three-belt event was identified,suggesting they played significant roles in the formation and evolution of the third *** injections may introduce new electron populations to the third belt,whereas ULF waves may influence the evolution of the third belt through radial *** the end of the three-belt event,the compression of the magnetosphere by shocks may lead to the dropout of the third belt because of the magnetopause shadowing effect and outward radial diffusion,ultimately disrupting the three-belt *** study provides more evidence for the presence of a sub-relativistic electron three-belt structure and offers an analysis of the evolutionary mechanisms of the third belt,which may contribute to a comprehensive understanding of the electron three-belt structure in the radiation belts.

关键词： belt Earth storm

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Comparison between the ring current energy injection and decay under southward and northward IMF Bz conditions during geomagnetic storms

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Science China(Technological Sciences) 2012年第10期55卷 2769-2777页

作者： SHI XiaoFei ZONG QiuGang WANG YongFu Institute of Space Physics and Applied Technology Peking UniversityBeijing 100871China

The geomagnetic storm is one of the most important geomagnetic disturbance phenomena in the *** studies assume that input of solar wind energy into the Earth's ring current only occurs when IMF Bz in GSM coordinates is southward;the ring current energy injection and decay under northward IMF Bz are not well understood and still need further *** this paper,by using the large amount of data from the year 1964 to 2010,we use the empirical phase space analysis method to study the ring current energy injection and decay under northward IMF Bz and compare the results with those under southward IMF Bz *** have found that the largest injection Q under northward IMF Bz condition is only 7% of the largest injection under southward IMF Bz,implying that there is a very limit energy injected into the ring current region when IMF Bz is *** decay time decreases as VBz increases and shows a good linear trend for southward IMF Bz;while for the northward IMF Bz,there is not a clear relation between τ varies and *** taken τ as a function of injection Q instead of VBz,we have obtained the empirical relation of τ with Q for northward and southward IMF Bz conditions:the two categories are further combined together and the empirical relation τ= e(2.6 0.039 Q) is ***,the pressure-corrected Dst formula Dst=Dst b P+c is derived for both southward and northward IMF Bz conditions,where the coefficients b and c are 6.9/10.4 and 10.0/15.2 when IMF Bz is southward and northward *** statistical results on between the different geomagnetic indices(Dst,Kp,AE) and IMF Bz are also obtained.

关键词： pressure-corrected Dst index decay time energy injection

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Ultra low frequency waves impact on radiation belt energetic particles

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Science China(Technological Sciences) 2009年第12期52卷 3698-3708页

作者： ZONG QiuGang HAO YongQiang WANG YongFu Institute of Space Physics and Applied Technology Peking UniversityBeijing 100871China

One of the most fundamental important issues in the space physics is to understand how solar wind energy transports into the inner *** low frequency(ULF)wave in the magnetosphere and its impact on energetic particles,such as the wave-particle resonance,modulation,and particle acceleration,are extremely important topics in the Earth’s radiation belt dynamics and solar wind― magnetospheric *** this review,we briefly introduce the recent advances on ULF waves study. Further,we will explore the density structures and ion compositions around the plasmaspheric boundary layer(PBL)and discuss its possible relation to the ULF waves.

关键词： radiation belt particle ULF wave wave-particle interaction(WPI) energetic particles acceleration plasmaspheric boundary layer oxygen ions

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Dynamic variations of the outer radiation belt during magnetic storms for 1.5–6.0 MeV electrons

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Science China(Technological Sciences) 2011年第2期54卷 431-440页

作者： YUAN ChongJing ZONG QiuGang Institute of Space Physics and Applied Technology Peking University Beijing 100871 China

The CME’s structure of solar wind(interplanetary magnetic field)is different from CIR’*** two processes in which plasma and solar wind energy are injected into the Earth’s inner magnetosphere are not the ***,the variations of energetic elec- trons flux in the radiation belts are different between the storms associated with CMEs and *** using data from SAMPEX(Solar,Anomalous,and Magnetospheric Particle Explorer)satellite,we have investigated the dynamic variations of the outer radiation belt for 1.5–6.0 MeV electrons during 54 CME-driven storms and 26 CIR-driven recurrent *** to the superposed epoch analysis,for CME-and CIR-driven storms,when the Dst index reaches the minimum,the locations of the outer boundary move to L=4 and L=5.5,*** the recovery phases,the locations of the outer boundary of the outer radiation belt are generally lower than and slightly higher than those before CME-and CIR-driven storms,*** have found that the logarithmically decaying 1/e cut-off L-shell is a satisfying indicator of the outer boundary of the outer radiation ***,our study shows that the logarithmically decaying 1/e cut-off latitude is dependent on the Kp index in the main phases of CME-and CIR-driven storms,while in the recovery phases,there is no obvious *** ad- dition,it has been shown that the locations of the peak electron flux are controlled by the minimum Dst index in the main phases of CME-driven *** influences of multiple storms on the electron flux of outer radiation belt have also been in- vestigated.

关键词： outer radiation belt relativistic electrons magnetic storms CME CIR energetic particles

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Discrete energetic(～50-200 keV) electron events in the high-altitude cusp/polar cap/lobe

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Science China(Technological Sciences) 2017年第12期60卷 1935-1940页

作者： WANG LingHua ZONG QiuGang SHI QuanQi WANG YongFu TU ChuanYi HE JianSen TIAN Hui WIMMER-SCHWEINGRUBER Robert F. ZOU Hong Institute of Space Physics and Applied Technology Peking University Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment School of Space Science and PhysicsShandong University Institute for Experimental and Applied Physics University of Kiel

We identified 28 discrete electron events(DEEs) with enhanced fluxes at ~50-200 keV in the high-altitude cusp/polar cap/lobe,using the electron measurements by the BeiDa Image Electron Spectrometer(BD-IES) instrument onboard an inclined(55°)geosynchronous orbit(IGSO) satellite from October 2015 to January 2016. We find that among the 28 DEEs, 22 occur in the nightside and mostly in the northern cusp/polar cap/lobe, while 6 occur in the dayside and all in the southern cusp; 24 events correspond to an average interplanetary magnetic field(IMF) component B_z>0, 3 correspond to an average IMF B_z<0, and 1 has no OMNI IMF data. In these DEEs, the observed average omnidirectional electron differential flux generally fits well to a power-law spectrum, J^E^(-γ), with the spectral index y ranging from 2.6 to 4.6, while the average electron flux varies over three orders of magnitude from event to event. The spectral index of these cusp DEEs are(strongly) larger than the spectral index of solar wind superhalo electrons(radiation belt electrons) observed by the WIND 3 D Plasma & Energetic Particle instrument(the BD-IES). At^110 keV,the electron flux of DEEs in the cusp/polar cap/lobe shows a weak positive correlation with the solar wind superhalo electron flux but no obvious correlation with the radiation belt electron flux. These results suggest that these DEEs probably originate from transient processes acting on the solar wind superhalo electrons, e.g., the mid/high-latitude reconnection.

关键词： energetic electrons energetic particles acceleration solar wind superhalo electrons

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