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| 1 | The state-of-the-art of the China Seismo-Electromagnetic Satellite mission显示文摘The China Seismo-Electromagnetic Satellite(CSES) mission was proposed in 2003 and approved in 2013 after ten years' scientific and engineering demonstrations. To meet the requirement of scientific objectives, the satellite is designed to be in a sunsynchronous orbit with an altitude of 507 km and descending node time of 14:00 LT. The CSES satellite carries 8 instruments,including search-coil magnetometer(SCM), electric field detector(EFD), high precision magnetometer(HPM), GNSS occultation receiver(GOR), plasma analyzer package(PAP), langmuir probe(LAP), high energetic particle package(HEPP) and detector(HEPD), and tri-band beacon(TBB), among which HEPD is provided by Italian Space Agency. The CSES satellite was launched successfully on February 2, 2018, and is planned to operate for 5 years. The CSES mission is the first satellite in China to measure geophysical fields, which will have a lot of application prospects in the study of seismology, geophysics, space sciences, and so on. | SHEN XuHui ZHANG XueMin YUAN ShiGeng WANG LanWei CAO JinBin HUANG JianPing ZHU Xing Hong PIERGIORGIO Picozzo DAI JianPing | 2018 | Science China(Technological Sciences)2018，61，5： | 33 |
| 2 | The electromagnetic wave experiment for CSES mission: Search coil magnetometer显示文摘The seismic activities on the Earth can produce a disturbance of the electromagnetic field and particles in the ionosphere. The search coil magnetometer(SCM) mounted on China Seismo-Electromagnetic satellite(CSES) is designed to measure the magnetic field fluctuation of low frequency electromagnetic waves in the frequency range of 10 Hz–20 k Hz. The SCM comprises a three-axis search coil sensor mounted on a 4.5 m boom and an electronic box inside satellite module. The sampling rate of the SCM is 51.2 k Hz and the time resolution of the power spectrum density(PSD) is 2 s. The frequency resolution is 12.5 Hz.There are three operation modes: survey, detailed survey and calibration. In the survey mode, the SCM can provide a PSD in the whole frequency range of 10 Hz–20 k Hz and wave forms in the low frequency range below 2 k Hz while in the detailed survey mode the SCM can provide both PSD and wave forms in the whole frequency range of 10 Hz–20 k Hz. The sensitivity of the SCM instrument is 5.0×10^(-4) n T Hz^(-1/2) at 10 Hz, 5.0×10^(–5) n T Hz^(-1/2) at 200 Hz, 3.4×10^(-5) n T Hz^(-1/2) at 2 k Hz and 1.1×10^(-4) n T Hz^(-1/2) at 20 k Hz. The telemetry rate is ~0.85 Mbps in the survey mode and ~3.0 Mbps in the detailed survey mode. The phase difference between three axes can be made generally with a precision of less than 1.0°. The dynamic range of the SCM instrument is over 100 d B. The orthogonality of three mechanical axes of search coil senor is better than 0.13°. The performance of SCM can satisfy the requirement of scientific objectives of CSES mission. | CAO JinBin ZENG Li ZHAN Feng WANG ZuoGui WANG Yan CHEN Yu MENG QingChun JI ZhanQiang WANG PengFei LIU ZhongWei MA LingYu | 2018 | Science China(Technological Sciences)2018，61，5： | 13 |
| 3 | Differences between onset times of bursty bulk flows (BBFs) of two Cluster satellites in the magnetotail显示文摘This paper using the dataset of BBFs (bursty bulk flows) observed by two Cluster satellites C1 and C4 studies the difference between onset times of BBFs observed by C1 and C4. It is found that the onset time differences of most of BBFs observed by C1 and C4 are smaller than 60 s. The average onset time difference of BBFs of C1 and C4 is 68.5 s. The probabilities of onset time difference of BBFs of C1 and C4 larger than 30 60 90 and 120 s are respectively 55% 35% 27% and 23%. The largest onset time difference of BBFs of C1 and C4 decreases with the increase of earthward component of maximum velocities of BBFs. The onset time difference of BBFs of C1 and C4 results from the velocity inhomogeneity inside the flow channel of BBF which may be produced in propagation path and/or in source region of BBFs. Such a wide range of onset time difference of BBFs suggests that the velocity inhomogeneity inside the flow channel of BBF is various. These results are very important to the current study of substorm research based on THEMIS data because they indicate that it is impossible to determine the onset time of BBF with a single satellite. | CAO JinBin WANG ZhiQiang MA YuDuan CAI CunLin | 2012 | Science China(Technological Sciences)2012，55，5： | 8 |
| 4 | Multi-spacecraft observations of earthward flow bursts显示文摘On the basis of the plasma, electric and magnetic fields jointly observed by Cluster and the Double Star TC-1 spacecraft in the Earth's magnetotail, we have investigated the earthward flow bursts by introducing the momentum equation in the X-direction in the ideal conditions of magneto hydrodynamics (MHD). One earthward flow burst with a peak in excess of 500 km/s was selected, when the four spacecraft of Cluster were located around ?16 RE and TC-1 was located around ?10 RE in the X-direction. The inter-spacecraft distances in Y and Z directions were smaller than the statistical spatial scales of the bursty bulk flows. When the Y components of E and ?V×B were compared, there was no clear breakdown of the frozen-in condition during the earthward flow burst. With the measured plasma and magnetic parameters from two spacecraft at different positions in the magnetotail, the X component of the pressure gradient was calculated. Magnetic tension was calculated using the magnetic field measured at four points, which could be compared with the assumed constant in the past research with single satellite. When the pressure gradient and the magnetic tension were put into the MHD momentum equation, some samples of the earthward flow bursts were accelerated and some were decelerated. The braking process of the earthward flow burst was more complicated than what the past results had shown. The accelerated samples accounted for about one third of the whole earthward flow bursts and discontinuously located among the decelerated elements. The original single earthward flow burst event might be split into several short flow bursts when it was moving to the Earth. Our results may partly illustrate that the duration of fast flows during three phases of substorm becomes short near the Earth. The results are consistent with the past results that fast flows intrude to places earthward the typical braking region. | MA YuDuan CAO JinBin REME Henry DANDOURAS Iannis DUNLOP Malcolm LUCEK Elisabeth | 2012 | Science China(Technological Sciences)2012，55，5： | 8 |
| 5 | MHD and kinetic analysis of flow bursts in the Earth's plasma sheet显示文摘In an attempt to study the flow bursts in the Earth’s plasma sheet we select an event that took place on August 7,2004 in the expansion phase of a substorm,using data from the geomagnetic index,solar wind data,plasma and magnetic field observations from C1 Cluster satellite(the Cluster mission has 4 satellites)and from Double Star TC-1 satellite.In MHD approach,TC-1 firstly observed the tailward flow,then the earthward,and finally the flow alternated in two directions.C1 firstly observed the earthward plasma flow,and then the tailward plasma flow.Before flow bursts are observed by TC-1 and C1,there are disturbances in local entropy with their tailward local entropy larger than those of the earthward.The kinetic features of the plasma flow observed by C1 are similar to those in MHD.However,kinetic characteristics of the plasma flow observed by TC-1 are far more than the description in MHD.The inadequacy mainly exists in two cases:(i)the firstly enhanced tailward flows given in MHD are found without significant increase of the energetic tailward flux;(ii)the almost stagnant flow in MHD is composed of the enhanced energetic ion flux in both earthward and tailward directions.The earthward flow burst observed by TC-1 might be multiple overshoots and rebounds.The earthward flow burst observed by C1 might be simply rebounded in the near-Earth.The pulsation observed by C1 is earlier than that observed by TC-1 with the former intensity less than that of the latter.After the energetic ion flux in the tailward direction is significantly enhanced,the power spectrum intensity of the ULF wave commences to increase obviously,which may suggest that the stream instability is closely correlated with ULF pulsations. | MA YuDuan CAO JinBin FU HuiShan REME H. DANDOURAS I. YANG JunYing WANG ZhiQiang TAO Dan YANG Jian | 2014 | Science China(Technological Sciences)2014，57，1： | 7 |
| 6 | Cluster observations of large-scale southward movement and dawnward-duskward flapping of Earth's magnetotail current sheet显示文摘In August 2001,Cluster satellites observed that the mid-tail current sheet(CS) moved southward continuously for almost seven hours.Meanwhile,Cluster crossed back and forth the CS repeatedly.This means that the large-scale southward movement of the CS was accompanied by a small-scale CS flapping during this period.Using the minimum-variation-analysis(MVA) method and the multi-spacecraft data,we calculated the normal vector,current density and the magnetic curvature of the CS,the results showed that the CS alternated between flattened CS and tilted CS for several times.Strong dawn-dusk oscillations were found for the tilted CS,which caused the repeated crossings of the center of CS by the satellites.This feature is obviously different from the previous observations of the vertical flapping of the CS induced by the kink instability.Two types of flapping were observed:One of them is accompanied with bursty bulk flows(BBFs) and the other is not.This suggests that in this event there was no direct relationship between the CS flapping and BBFs. | DUAN AiYing CAO JinBin MA YuDuan WEI XinHua | 2013 | Science China(Technological Sciences)2013，56，1： | 6 |
| 7 | The mid-high latitude whistler mode chorus waves observed around substorm onsets显示文摘Using the data of LFEW/TC-2, we studied the dawn side chorus around substorm onsets during a strong geomagnetic storm in November 2004. During this storm, LFEW/TC-2 observed 14 dawnside chorus events. Nine of them were associated with substorms and occurred within 40 min around the substorm onsets. The fre-quencies of waves have a very good correlation with the half equatorial electron cyclotron frequencies. Chorus can be excited in the region near magnetic equato-rial plane and then propagate to the mid and high latitudes. When the wave fre-quencies reach the local lower hybrid frequencies, chorus can be reflected due to the lower hybrid resonance. The time delay between the chorus and its echo is about 28 min. Previous observations show that the chorus can propagate at most to the magnetic latitudes of 40°. LFEW/ TC-2 found for the first time that the chorus in space could propagate to the magnetic latitude of 70°. Since most of the previous chorus observations are made close to the magnetic equatorial plane, our results are important for the studies of excitation and propagation of whistler mode wave, and relevant relativistic electron acceleration in the magnetosphere. | YANG JunYing CAO JinBin YAN ChunXiao LI LiuYuan MA YuDuan | 2008 | Science China(Technological Sciences)2008，51，10： | 6 |
| 8 | The causal sequence investigation of the ring current ion-flux increasing and the magnetotail ion injection during a major storm显示文摘全面记录在 NUADU 仪器在主要磁性的暴风雨期间在 2005 年 5 月 15 日在 TC-2 上记录的戒指水流活动的 ENA 数据是可得到的(它合并了一系列 substorms ) 。在时间的分辨率在 5081 和 81158 keV 与相比的精力范围从 ENA 数据导出的 4-min 的离子流动在 situ ,粒子流动在 LANL-01 上由 LANL-SOPA 仪器测量了, LANL-02 , LANL-97 ,并且 LANL-84 (环绕的一系列地球同步的卫星在~的赤道的飞机 6.6 R E )。另外,磁场在 GOES-10 和 GOES-12 上由 magetometers 同时测量了(它也是地球同步的卫星) 与粒子数据相比。在戒指水流的离子流动在在 substorms 而非在向地的指导 dipolarization 事件以后的生长阶段拉长的地磁气的地 tailward 期间被提高,这被表明。这观察,它质问戒指水流粒子被注射的存在概念从 magnetotail 追随者 dipolarization 事件向地,用很多磁性的暴风雨事件要求进一步的调查。 | LU Li S MCKENNA-LAWLOR CAO JinBin K KUDELA J BALAZ | 2016 | Science China Earth Sciences2016，59，1： | 4 |
| 9 | New progress of Double Star-Cluster joint exploration and study显示文摘The magnetic reconnection of magnetosphere and the magnetospheric space storms (including magnetospheric substorm, magnetic storm, magnetospheric particle storm) has long been one of the most challenging subjects in the so-lar-terrestrial physics. The reconnection mechanism and global triggering process of the magnetospheric space storms are still unclear up to now. Based on the Double Star Program (DSP) and Cluster joint measurements, we have observed the solar wind density hole, the component magnetic field reconnection in the magnetopause, the structures of magnetic storm ring current, global and multi-scale driven and triggering processes of magnetospheric substorm. In this paper we will briefly introduce these results. | LIU ZhenXing PU ZuYin CAO JinBin SHEN Chao LU Li ZHANG LingQian | 2008 | Science China(Technological Sciences)2008，51，10： | 4 |
| 10 | In-flight observations of electromagnetic interferences emitted by satellite显示文摘Using the data from STAFF/TC-1, this paper for the first time analyzes the electromagnetic interferences of Chinese scientific satellite. The electromagnetic interference of satellite exists mainly below 30 Hz, but can extend to 190 Hz with an obviously decreasing power spectral density. The electromagnetic interferences at frequencies below 190 Hz have good correlation with the solar aspect angle. The electromagnetic interferences at frequencies between 190 and 830 Hz have also correlation with solar as-pect angle. However, the electromagnetic interferences at frequencies above 830 Hz have no correlation with the solar aspect angle. The correlation coefficient between solar aspect angel and electromagnetic interferences is around 0.90. The larger the solar aspect angle, the stronger the satellite electromagnetic interference. When the solar aspect angle increases from 90.6° to 93.6°, the electromagnetic interferences at frequencies <10 Hz increase by 8 times and those at frequencies 190―830 Hz increase by 60%. This close association of electromagnetic interferences with the solar aspect angle indicates that the solar aspect angle is the main factor to determine the electromagnetic interferences. The electromagnetic interferences of satellite in sunlight are larger than those in eclipse. The electro-magnetic interference produced by solar panel occupies about 87% in the low frequency band (<100 Hz) and 94% in the high frequency band (>100 Hz) of the total electromagnetic interference produced by satellite. These in flight observations of electromagnetic radiation of satellites will be very helpful to the designs of future satellites of space sciences or earthquake sciences. | CAO JinBin YANG JunYing YUAN ShiGan SHEN XuHui LIU YuanMo YAN ChunXiao LI WenZhen CHEN Tao | 2009 | Science China(Technological Sciences)2009，52，7： | 4 |
| 11 | Plasma sheet stretching accompanied by field aligned energetic ion fluxes observed by the NUADU instrument aboard TC-2显示文摘NUADU (中立原子察觉者单位) 在 TC-2 上的仪器记录了在 thenear 地球血浆表盘旋在磁场线附近的控告的粒子(E>180 keV ) 的 4nsolid 角度图象(在 ~-7 R_E,赤道的 dawn-to-night 方面) 在地磁气的暴风雨(Dst=-219 nT ) 期间在 2005 年 8 月 24 日。对称的、似环的、稳固的角度分布在周围的磁场线附近描绘的精力充沛的离子横梁事件被 theTC-2 太空船在血浆表的 34-minutetraversal 期间观察。另外,观察被磁强计实验(FGM ) 在一样的太空船上在血浆表的这些多重十字路口期间监视。在每个十字路口期间,口哨声模式合唱团改进被 TC-2 低频率电磁波察觉者(LFEW/TC-2 ) 就在本地更低的混血儿的上面在频率在各向异性的区域观察波浪。离子的比较与这块地里的改进排列了的周围的磁场表演搭角度分发(垫) 地图精力充沛的离子流动被尾巴病房在血浆表拉长磁场线伴随。相反,垂直离子流动改进被在血浆表显示磁场线的相应收缩的签名伴随。因为平行离子流动和垂直离子流动改进间歇地发生了,数据被解释暗示磁场线的一个动态、摆动的过程(拉长并且缩小)在thenear地球血浆表,它可能行动了帮助在将支持在进行中的磁性的暴风雨期间被触发的连续 aurora-substorm 的这个区域建立一个相互作用区域。Thewhistler 模式合唱团可能在血浆表压缩以后在粒子沥青角度散开期间由于离子旋转罗盘回声被生产了。 | LU Li S. MCKENNA-LAWLOR S. BARABASH LIU ZhenXing CAO JinBin J. BALAZ K. KUDELA T. L. ZHANG C. M. CARR | 2007 | Chinese Science Bulletin2007，52，12： | 4 |
| 12 | Response of magnetic fields at geosynchronous orbit and on the ground to the sudden changes of IMF B_Z显示文摘The rapid change in the Earth’s magnetosphere caused by solar wind disturbances has been an important part of the solar wind-magnetosphere interaction.However most of the previous studies focused on the perturbation of the Earth’s magnetic field caused by solar wind dynamic pressure changes.In this paper,we studied the response of geosynchronous magnetic field and the magnetic field to the rapid southward turning of interplanetary magnetic field during the interval 1350 1420 UT on 7May 2007.During this event,BZ component of the interplanetary magnetic field decreased from 15 nT to 10 nT within 3 min(1403 1406 UT).The geosynchronous magnetic field measured by three geosynchronous satellites(GOES 10 12)first increased and then decreased.The variations of magnetic field strength in the morning sector(9 10 LT)were much larger than those in the dawn sector(5 LT).Meanwhile,the H components of geomagnetic field on the ground have similar response features but exhibit latitude and LT dependent variations.Compared with H components,the D components do not have regular variations.Although the solar wind dynamical pressure encounters small variations,the magnetic field both in space and on the ground does not display similar variations.Therefore,the increase of geomagnetic field in the dawn sector is caused by the southward turning of IMF(interplanetary magnetic field)BZ.These results will help to better understand the coupling process of geomagnetic filed and interplanetary magnetic field. | DONG YiXuan CAO JinBin LIU WenLong ZHANG Lei LI LiuYuan | 2014 | Science China(Technological Sciences)2014，57，2： | 3 |
| 13 | Ionospheric TEC and plasma anomalies possibly associated with the 14 July 2019 M_(w) 7.2 Indonesia Laiwui earthquake,from analysis of GPS and CSES data显示文摘This study presents signatures of seismo-ionospheric perturbations possibly related to the 14 July 2019 M_(w)7.2 Laiwui earthquake,detected by a cross-validation analysis of total electron content(TEC)data of the global ionospheric map(GIM)from GPS and plasma parameter data recorded by the China Seismo-Electromagnetic Satellite(CSES).After separating pre-seismic ionospheric phenomena from the ionospheric disturbances due to the magnetospheric and solar activities,we have identified three positive temporal anomalies,around the epicenter,at 1 day,3 days and 8 days before the earthquake(14 July 2019),along with a negative anomaly 6 days after the earthquake.These results agree well with the TEC spatial variations in latitude-longitude-time(LLT)maps.To confirm these anomalies further,we employed the moving mean method(MMM)to analyze ionospheric plasma parameters(electron,O^(+) and He^(+) densities)recorded by the Langmuir probe(LAP)and Plasma Analyzer Package(PAP)onboard the CSES.The analysis detected on,on Day Two,Day Four,and Day Seven before the earthquake,remarkable enhancements along the orbits around when in proximity to the epicenter.To make the investigations still more convincing,we compared the orbits on which anomalous readings were recorded to their corresponding four nearest revisiting orbits;the comparison did indeed indicate the existence of plasma parameter anomalies that appear to be associated with the Laiwui earthquake.All these results ilustrate that the unusual ionospheric perturbations detected through GPS and CSES data are possibly associated with the M_(w)7.2 Laiwui earthquake,which suggests that at least some earthquakes may be predicted by alertness to pre-seismic ionospheric anomalies over regions known to be at seismic risk.This case study also contributes additional information of value to our understanding of lithosphere-atmosphere-ionosphere coupling. | YuanZheng Wen Dan Tao GuangXue Wang JiaYi Zong JinBin Cao Roberto Battiston ZhiMa ZeRen XuHui Shen | 2022 | Earth and Planetary Physics2022，6，4： | 3 |
| 14 | Spatial distribution of ion polytropic index joint-modulated by temperature anisotropy and MHD disturbances in the southern high latitude magnetosheath显示文摘Using the Cluster data from 2001 to 2010, we studied spatial distribution of effective ion polytropic index in the southern high latitude magnetosheath, and joint-modulation of ion polytropic index by temperature anisotropy and MHD disturbances. The magnetosheath ions generally experience various polytropic processes with different polytropic index. The median polytropic indexes of magnetosheath ions in the GSE X-Y plane decrease toward the bow shock. Near the magnetopause, the median polytropic indexes are basically between isothermal and adiabatic except in the duskside flank close to the terminator. The analysis of correlation coefficient of perturbed ion number density with parallel magnetic field CC_δnδB_‖ and ion temperature anisotropy parameter A_T, indicates that the dominant MHD disturbance near magnetopause is slow mode with larger ion temperature anisotropy, and there are various modes of MHD disturbances with insignificant ion temperature anisotropy near the bow shock.The polytropic index modulated by slow mode disturbances is generally larger than that modulated by fast mode disturbances, and the larger ion temperature anisotropy, the larger polytropic index. The median polytropic indexes modulated jointly by slow mode disturbances and the strong ion temperature anisotropy can be larger than 1.0, while those modulated by fast mode disturbances and weak temperature anisotropy can be even possibly close to zero. Moreover, because of pronounced dusk-favored asymmetry of ion temperature anisotropy, the median polytropic index in the dawnside flank of the magnetosheath near the terminator is smaller than that in the duskside flank of the magnetosheath. The good correspondence between the distributions of median polytropic indexes and ion temperature anisotropy and MHD disturbances indicates that the ion temperature anisotropy and MHD disturbances determine the distribution of the polytropic index in the magnetosheath. | PANG XueXia CAO JinBin DENG ZeChao JIA PengYing | 2018 | Science China(Technological Sciences)2018，61，3： | 2 |
| 15 | China Seismo-Electromagnetic Satellite search coil magnetometerdata and initial results显示文摘Four levels of the data from the search coil magnetometer(SCM) onboard the China Seismo-Electromagnetic Satellite(CSES)are defined and described. The data in different levels all contain three components of the waveform and/or spectrum of the induced magnetic field around the orbit in the frequency range of 10 Hz to 20 kHz; these are divided into an ultra-low-frequency band(ULF,10–200 Hz), an extremely low frequency band(ELF, 200–2200 Hz), and a very low frequency band(VLF, 1.8–20 kHz). Examples of data products for Level-2, Level-3, and Level-4 are presented. The initial results obtained in the commission test phase demonstrated that the SCM was in a normal operational status and that the data are of high enough quality to reliably capture most space weather events related to low-frequency geomagnetic disturbances. | Qiao Wang JianPing Huang XueMin Zhang XuHui Shen ShiGeng Yuan Li Zeng JinBin Cao | 2018 | Earth and Planetary Physics2018，2，6： | 2 |
| 16 | Case study of small scale polytropic index in the central plasma sheet显示文摘This paper studies the effective polytropic index in the central plasma sheet(CPS) by using the method of Kartalev et al.(2006), which adopts the denoising technique of Haar wavelet to identify the homogeneous MHD Bernoulli integral(MBI) and has been frequently used to study the polytropic relation in the solar wind. We chose the quiet CPS crossing by Cluster C1 during the interval 08:51:00–09:19:00 UT on 03 August 2001. In the central plasma sheet, thermal pressure energy per unit mass is the most important part in MBI, and kinetic energy of fluid motion and electromagnetic energy per unit mass are less important. In the MBI, there are many peaks, which correspond to isothermal or near isothermal processes. The interval lengths of homogenous MBI regions are generally less than 1 min. The polytropic indexes are calculated by linearly fitting the data of lnp and lnn within a 16 s window, which is shifted forward by 8 s step length. Those polytropic indexes with |R|≥0.8(R is the correlation coefficient between lnp and lnn) and p-value≤0.1 in the homogeneous regions are almost all in the range of [0, 1]. The mean and median effective polytropic indexes with high R and low p-value in homogeneous regions are 0.34 and 0.32 respectively, which are much different from the polytropic index obtained by traditional method(?trad=?0.15). This result indicates that the CPS is not uniform even during quiet time and the blanket applications of polytropic law to plasma sheet may return misleading value of polytropic index. The polytropic indexes in homogeneous regions with a high correlation coefficient basically have good regression significance and are thus credible. These results are very important to understand the energy transport in magnetotail in the MHD frame. | PANG XueXia CAO JinBin LIU WenLong MA YuDuan LU HaoYu YANG JunYing LI LiuYuan LIU Xu WANG Jing WANG TieYan YU Jiang | 2015 | Science China Earth Sciences2015，58，11： | 2 |
| 17 | Wavenumber-4 spectral component extracted from TIMED/SABER observations显示文摘The wavenumber spectral components WN4 at the mesosphere and low thermosphere(MLT)altitudes(70–10 km)and in the latitude range between±45°are obtained from temperature data(T)observed by the Sounding of the Atmosphere using Broadband Emission Radiometry(SABER)instruments on board the National Aeronautics and Space Administration(NASA)’s Thermosphere–Ionosphere–Mesosphere Energetics and Dynamics(TIMED)spacecraft during the 11-year solar period from 2002 to 2012.We analyze in detail these spectral components WNk and obtain the main properties of their vertical profiles and global structures.We report that all of the wavenumber spectral components WNk occur mainly around 100 km altitude,and that the most prominent component is the wavenumber spectral component WN4 structure.Comparing these long duration temperature data with results of previous investigations,we have found that the yearly variation of spectral component WN4 is similar to that of the eastward propagating non-migrating diurnal tide with zonal wavenumber 3(DE3)at the low latitudes,and to that of the semi-diurnal tide with zonal wavenumber 2(SE2)at the mid-latitudes:the amplitudes of the A4 are larger during boreal summer and autumn at the low-latitudes;at the mid-latitudes the amplitudes have a weak peak in March.In addition,the amplitudes of component WN4 undergo a remarkable short period variation:significant day-to-day variation of the spectral amplitudes A4 occurs primarily in July and September at the low-latitudes.In summary,we conclude that the non-migrating tides DE3 and SE2 are likely to be the origins,at the low-latitudes and the mid-latitudes in the MLT region,respectively,of the observed wavenumber spectral component WN4. | Xing Li WeiXing Wan JinBin Cao ZhiPeng Ren | 2020 | Earth and Planetary Physics2020，4，5： | 1 |
| 18 | The response of plasma parameters and energy transport in the plasma sheet to interplanetary magnetic field B_z显示文摘We use 9 years data of Cluster to study the dependencies of plasma parameters and energy transport in the plasma sheet on the lasting time of northward/southward interplanetary magnetic field(IMF). The plasma parameters and energy transport in the plasma sheet always respond to the change of IMF direction by more or less time. The ion density starts to increase/decrease remarkably at 80 min after northward/southward IMF turning. The ion temperature starts to decrease at 25 min after northward IMF turning, whereas it starts to increase at 80 min after southward IMF turning. The earthward convection velocity within15 min after northward IMF turning almost equals to that within 15 min period after southward IMF turning. However at time greater than 15 min after southward IMF turning, the earthward convection velocity under southward IMF starts to remarkably increase. The response time(15 min) of magnetospheric convection velocity is well consistent with the response times of nightside ionospheric convection to southward IMF turning. The enthalpy flux is larger than kinetic flux by about three orders of magnitudes, and thus the enthalpy flux plays a dominant role in the plasma sheet energy transport. The enthalpy flux does not weaken immediately after northward IMF turning. The enthalpy flux within 15 min after northward IMF turning is comparable to or even slightly larger than that within 15 min after southward IMF. The enthalpy flux starts to decrease at times greater than15 min after northward IMF turning, whereas it starts to increase at times greater than 15 min after southward IMF turning. The result that the enhanced energy transport during the 15 min period after northward IMF turning may explain previous observation that substorms frequently occur shortly after northward IMF turning. | REN GanMing CAO JinBin YANG Jian DUNLOP Malcolm Wray | 2021 | Science China(Technological Sciences)2021，64，7： | 1 |
| 19 | MAGNETOSPHERIC PHYSICS IN CHINA:2000-2002显示文摘This brief report presents the latest advances of the magnetospheric physics researches in China during the period of 2000-2002, made independently by Chinese space physicists and through international cooperation. The related areas cover almost every aspect of magnetospheric physics. | CAO Jinbin LIU Zhenxing PU Zhuyin | 2002 | 空间科学学报2002，22，z1： | 1 |
| 20 | On the ion distributions at the separatrices during symmetric magnetic reconnection显示文摘A particle-in-cell simulation of symmetric reconnection with zero guide field is carried out to understand the dynamics of ions along the separatrices.Through the investigation of ion velocity distributions at different moments and locations along the separatrices,a typical distribution is found:two counter-streaming populations in the perpendicular direction,with another two populations accelerated into distinct energy levels in the parallel direction.Backward tracing of ions reveals that the counter-streaming cores are mostly composed of ions initially located at the same side of the separatrix,while the other two accelerated populations in the parallel direction are composed of ions crossing through the neutral sheet.Through analysis of energy conversion of these populations,it is found that the ion energization along the separatrix is attributable primarily to the Hall electric field,while that in the region between the two separatrices is caused primarily by the induced reconnection electric field.For the counter-streaming population,the low-energy ions that cross the separatrix twice are affected by both Hall and reconnection electric fields,while the high-energy ions that directly enter the separatrix from the unperturbed plasma are energized mainly by the Hall electric field.For the two energized populations in the parallel direction,the ions with lower-energy are accelerated mainly by the in-plane electric field and the Hall electric field on the opposite side of the separatrix,whereas the ions with higher-energy not only experience the same energization process but also are constantly accelerated by the reconnection electric field. | HongTao Huang YiQun Yu JinBin Cao Lei Dai RongSheng Wang | 2021 | Earth and Planetary Physics2021，5，2： | 1 |
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