Correlated observations linking loss of energetic protons to EMIC waves

Electromagnetic ion cyclotron (EMIC) emission is an efficient mechanism for scattering loss of energetic protons. Here, we report an event that provides both in-situ observation of energetic proton differential fluxes in the inner magnetosphere and precipitation of protons at ionospheric altitudes. During the 7–8 September 2015 geomagnetic storm the Van Allen Probes observed strong EMIC waves around L = 5 and a distinct decrement in fluxes of tens of keV protons around pitch angles 0°–45°. Meanwhile, precipitating protons at ionospheric altitudes were found to significantly enhanced (by several orders of magnitude), measured by NOAA 18 and 19 when they magnetically linked to the Van Allen Probe-A. By solving the Fokker-Planck diffusion equation, we show that EMIC waves can efficiently produce loss of energetic protons within about 2 h in the pitch angle range of ∼ 0°–45°, comparable to the satellite observations.

     

Variations of the relativistic electron flux after a magnetospheric compression event

On January 21, 2015, a sharp increase of the solar wind dynamic pressure impacted the magnetosphere. The magnetopause moved inward to the region L 8 without causing a geomagnetic storm. The flux of the relativistic electrons in the outer radiation belt decreased by half during this event based on the observations of the particle radiation monitor(PRM) of the fourth of the China-Brazil Earth Resource Satellites(CBERS-4). The flux remained low for approximately 11 d; it did not recover after a small magnetic storm on January 26 but after a small magnetic storm on February 2. The loss and recovery of the relativistic electrons during this event are investigated using the PRM data, medium-and high-energy electron observations of NOAA-15 and the Van Allen Probes, medium-energy electron observations of GOES-13, and wave observations of the Van Allen Probes. This study shows that the loss of energetic electrons in this event is related to magnetospheric compression. The chorus waves accelerate the medium-energy electrons, which causes the recovery of relativistic electrons. The Van Allen Probes detected strong chorus waves in the region L =3–6 from January 21 to February 2. However, the flux of medium-energy electrons was low in the region. This implies that the long-lasting lack of recovery of the relativistic electrons after this event is due to the lack of the medium-energy"seed" electrons. The medium-energy electrons in the outer radiation belt may be a clue to predict the recovery of relativistic electrons.     

通信基站风光互补发电系统的设计和研究

太阳能和风能作为两种应用广泛的可再生资源,在资源条件和技术应用上具有良好的互补性.风光互补发电可弥补单独风力和太阳能发电供电可靠性低和造价高等缺点,其应用领域广泛,可用于通讯中继站、市政亮化等场合.分析了风光互补发电系统的结构特点和运行原理,并在此基础上设计了通信基站的风光互补发电系统.     

某挠性卫星姿态控制系统设计

文中研究对象是带有太阳电池阵和天线等大挠性附件且太阳电池阵驱动的对地观测卫星.抑制太阳电池阵和天线挠性振动及太阳电池阵驱动对星体姿态影响是系统设计的目的.为此,选用带宽隔离法、坎值滤波器法对附件振动进行抑制;同时,针对卫星特殊飞行姿态所导致的通道间惯性耦合,设计了解耦算法给予解决;设计了具有低通滤波特性的外环修正回路,消除惯性基准单元的漂移误差及安装误差.将设计结果应用于对象模型并加入所有误差源后,进行仿真验证,系统设计结果满足给定的指标要求并有较大裕度.     

一次冷锋云系的宏微观物理特征分析

利用常规气象资料、自动站资料、卫星云图、CINRAD-SA多普勒天气雷达资料以及NCEP再分析资料,结合飞行探测数据,对影响2011年4月17日河北抚宁县森林大火的一次冷锋云系进行分析.结果表明:1)宏观分析,过程降水的水汽仅来自冷锋自身所携带的微弱水汽,水汽辐合值较小,不利降水;2)微观分析,冷锋层状云系在水平和垂直方向上存在较薄的过冷水云区,小粒子数浓度大于20cm-3的云区占一定比例.飞机催化作业后,雷达回波强度增强,CAS(云气溶胶粒子探头)探测的小粒子数浓度、云含水量及粒子平均直径均有明显变化,说明该次冷锋云系有一定的增雨潜力.     

Shrinkage of magnetosphere observed by TC-1 satellite during the high-speed solar wind stream

During the interval 06:14–07:30 UT on August 24, 2005, since the Earth’s magnetopause was suddenly compressed by the persistent high-speed solar wind stream with the southward component of the interplanetary magnetic field (IMF), the magnetopause moved inward for about 3.1 R_E. Meanwhile, TC-1 satellite shifted from northern plasma sheet to the northern lobe/mantle region, although it kept inward flying during the interval 06:00–07:30UT. The shift of TC-1 from the plasma sheet to the lobe/mantle is caused by the simultaneous inward displacements of the plasma sheet and near-Earth lobe/mantle region, and their inward movement velocity is larger than the inward motion velocity of TC-1. The joint inward displacements of the magnetopause, the lobe/mantle region and the plasma sheet indicate that the whole magnetosphere shrinks inward due to the magnetospheric compression by the high-speed solar wind stream, and the magnetospheric ions are attached to the magnetic field lines (i.e. ‘frozen’ in magnetic field) and move inward in the shrinking process of magnetosphere. The large shrinkage of magnetosphere indicates that the near-Earth magnetotail compression caused by the strong solar wind dynamic pressure is much larger than its thickening caused by the southward component of the IMF, and the locations of magnetospheric regions with different plasmas vary remarkably with the variation of the solar wind dynamic pressure. Supported by the National Natural Science Foundation of China (Grant Nos. 40604018, 40523006), CSSAR (Grant No. O72114AA4S), Scientific Research Start-up Foundation for President Prize of CAS, 973 Program of China (Grant No. 2006CB806305) and the Specialized Research Fund for State Key Laboratories     

水下爆炸气泡脉动的数值计算

水下近场爆炸可分为装药的爆轰、冲击波的产生和传播、气泡的形成和脉动.尽管气泡脉动压力峰值较冲击波小,但是近场水下爆炸气泡能量的衰减较冲击波慢,所以其对结构的影响却是不可忽视的.在充分考虑了能量的消耗,加入了虚拟力以及气泡能对整个气泡脉动特征的影响后,改进了水下爆炸引起气泡的脉动规律和水中压力分布规律的基本方程.利用采用龙格-库塔数值方法计算出了气泡的脉动直径、周期、速度和水中压力.所得计算结果与已有的各实验数据吻合良好.因此说明该方法对气泡脉动的描述非常符合真实情况.通过分析得出在近场时冲击波和气泡脉动压力波对于结构的破坏都有重要作用.     

Response of magnetic fields at geosynchronous orbit and on the ground to the sudden changes of IMF B Z

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.     

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

The CME’s structure of solar wind (interplanetary magnetic field) is different from CIR’s. The two processes in which plasma and solar wind energy are injected into the Earth’s inner magnetosphere are not the same. So, the variations of energetic electrons flux in the radiation belts are different between the storms associated with CMEs and CIRs. By 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 storms. According 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, respectively. In 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, respectively. We have found that the logarithmically decaying 1/e cut-off L-shell is a satisfying indicator of the outer boundary of the outer radiation belt. Furthermore, 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 correlation. In addition, 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 storms. The influences of multiple storms on the electron flux of outer radiation belt have also been investigated.

     

考虑预测不确定性的风-光-水多能互补系统调度风险和效益分析

风电、光伏与水电（简称风光水）互补发电系统是提高清洁能源整体利用效益的重要创新模式,随着风电、光伏发电渗透率的增加,如何解决大规模风光接入所带来的不确定性是多能互补系统研究的核心和难点。本文重点探讨日前风光出力预测的不确定性对于多能互补系统风险和效益的综合影响。首先,从可靠性、稳定性和经济性三个方面提出风光水多能互补系统调度运行风险和效益评价体系;建立多能互补系统短期优化调度模型,在日前风光出力预测结果基础上,编制系统日前发电计划;根据风光实际出力情况,滚动更新和模拟水电站实际调度过程。最后,对比分析各电站计划和实际调度运行情况,评价日前风光出力预测不确定性对于多能互补系统风险与效益的综合影响。本文以雅砻江流域锦屏一级多能互补系统为实例进行研究。相比风光水独立运行,风光水互补后系统的发电效益提高了37.13%,且系统出力过程更为稳定。互补系统在年尺度上具有良好的可靠性,但在水库低水位时期,系统失负荷天数明显增多,占全年失负荷天数的96%以上,系统可靠性降低;在汛期,互补后水库的下泄流量最大增加了47.06%,出现水量集中下泄的情况,这给电力部门、下游用水部门以及防护对象带来一定的防洪风险。     

基于统计降尺度方法的夏季降水精细化预报

利用1999—2009年安徽省淮河以南地区60个县市站夏季逐日降水资料和安庆市探空站逐日资料,研究了中低层不同风向配置下局地降水与大尺度降水场之间的关系,以3种不同预报对象及相应的预报因子分别采用神经网络和线性回归方法设计6种预报模型对观测资料进行逼近和优化,从而实现空间降尺度.分析对比6种预报模型46站逐日降水量的拟合和预报效果,结果表明:采取相同的预报对象及预报因子的BP神经网络模型在拟合和预报效果上均好于线性回归模型,可见夏季降水场之间以非线性相关为主;神经网络模型预报结果同常用的Cressman插值预报相比,能很好地反映出降水的基本分布及局地特征;预报对象为单站降水序列的神经网络模型在以平原、河流为主要地形的区域预报效果较好,预报对象为REOF主成分的神经网络模型则在山地和丘陵地形区域预报效果较好.     

An analysis of the correlation between the fluxes of high-energy electrons and low-middle-energy electrons in the magnetosphere

The variation of the flux of energetic electrons in the magnetosphere has been proven to be strongly related to the solar wind speed. Observations of GEO orbit show that the flux of low-energy electrons is not only modulated by the solar wind speed, but, if a time delay is added, is also positively correlated to the flux of high-energy electrons. This feature provides a possible method to forecast the flux of high-energy electrons in GEO orbit. In this study, the correlations of the fluxes between the high-energy electrons and low-middle-energy electrons obtained at different L values and in different orbits are investigated to develop the application of this feature. Based on the analysis of long–term data observed by NOAA POES and GOES, the correlations between the fluxes of high-energy electrons and low–middle–energy electrons are good enough at different L values and in different orbits in quiet time, but this correlation is strongly affected by CME–driven geomagnetic storms.     

Particle bursts in the inner radiation belt related to global lightning activity

Particle bursts (PBs), the phenomena characterized by short-term increases of particle counting rates (CRs), were observed by space-borne radiation belt particle detectors. With the electron CR data obtained by National Oceanic and Atmospheric Administration (NOAA)-18 satellite, the occurrence of PBs in the inner belt (1?L?2 and B?20.5 μT) were derived for years 2006–2011. The monthly occurrence number of PBs exhibits a strong maximum in northern summer (May–August). In association with global lightning data, the seasonal occurrence of PBs is found to be consistent with the lightning activity, especially if only lightning flashes at latitudes >20° are taken into account. The positive correlation between PBs and mid-latitude lightning discharges indicates the role of lightning-induced whistler waves, and is consistent with the expected pitch-angle scattering by wave-particle interactions. The contribution of lightning is so significant that it forms a non-negligible seasonal background of PBs. If one connects PBs to seismoelectromagnetic emissions (SEME) in attempt to find the earthquake precursor, the lightning background needs to be considered with great care.     

Research progress based on observations of the New Vacuum Solar Telescope

The purpose of this paper is to introduce the main scientific results made by the one-meter New Vacuum Solar Telescope(NVST),which was put into commission on 2010. NVST is one of the large aperture solar telescopes in the world, located on the shore of Fuxian lake of Yunnan province in China, aiming at serving solar physicists by providing them with high resolution photospheric and chromospheric observational data. Based on the data from NVST and complementary observations from space(e.g.,Hinode, SDO and IRIS, etc), dozens of scientific papers have been published with a wide range of topics concentrating mainly on dynamics and activities of fine-scale magnetic structures and their roles in the eruptions of active-region filaments and flares.The achievements include dynamic characteristics of photospheric bright points, umbral dots, penumbral waves, and sunspot/light bridge oscillation, observational evidence of small-scale magnetic reconnection, and fine-scale dynamic structure of prominences.All these new results will shed light on the better understanding of solar eruptive activities. Data release, observation proposals,and future research subjects are introduced and discussed.     

兆瓦级太阳能热气流发电站风荷载的数值模拟

针对发电功率为100 MW的太阳能热气流发电系统进行几何尺寸设计,运用计算流体力学(CFD)方法对兆瓦级太阳能热气流发电站的平均风荷载进行数值模拟,得到烟囱和集热棚内、外风场和风压分布规律.根据风工程理论计算烟囱表面的压力系数和风载体型系数,与规范中圆截面构筑物的体型系数以及相关结构的风洞试验值进行比较.结果表明,模拟值与规范值基本吻合,这说明运用CFD方法对超高耸结构进行风荷载模拟是可行的.绘制体型系数曲线,研究烟囱沿圆周方向和高度方向平均风荷载的分布规律,结果表明,圆截面高耸结构的体型系数随高度的增大而减小.     

LSTM-WBLS模型在日降水量预测中的应用

基于长短时记忆网络(Long Short-Term Memory, LSTM)降水量预测模型存在过拟合、时滞现象,而宽度学习系统(Broad Learning System, BLS)无需多次迭代的特点有助于解决LSTM的上述缺点.加权宽度学习系统(Weighted Broad Learning System, WBLS)通过在BLS中引入加权惩罚因子约束分配样本权重,降低噪声和异常值对降水量预测精度的影响.本文提出一种LSTM-WBLS日降水量预测模型,选取湖北省巴东站日降水量进行实证研究,并考虑气压、气温、湿度、风速和日照等因素对降水量的影响.实验结果表明,与现有的预测模型相比,LSTM-BLS模型在RMSE、MAE和R²等评价指标上均有显著提升.不同时间步长下,本文模型预测精度均优于现有模型,验证了其稳定性.与LSTM相比,WBLS直接计算权重的特点使得LSTM-WBLS的运算效率并未降低.     

Butterfly distribution of Earth’s radiation belt relativistic electrons induced by dayside chorus

Previous theoretical studies have shown that dayside chorus can produce butterfly distribution of energetic electrons in the Earth’s radiation belts by preferentially accelerating medium pitch angle electrons, but this requires the further confirmation from high-resolution satellite observation. Here, we report correlated Van Allen Probes data on wave and particle during the 11–13 April, 2014 geomagnetic storm. We find that a butterfly pitch angle distribution of relativistic electrons is formed around the location L = 4.52, corresponding to the presence of enhanced dayside chorus. Using a Gaussian distribution fit to the observed chorus spectra, we calculate the bounce-averaged diffusion rates and solve two-dimensional Fokker-Planck equation. Numerical results demonstrate that acceleration by dayside chorus can yield the electron flux evolution both in the energy and butterfly pitch angle distribution comparable to the observation, providing a further evidence for the formation of butterfly distribution of relativistic electrons driven by very low frequency (VLF) plasma waves.     

In-flight observations of electromagnetic interferences emitted by satellite

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 aspect 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 electromagnetic 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. Supported by the National Hi-Tech Research and Development Program of China (“863” Project) (Grant No. 2008AA12A216), the National Science & Technology Supporting Program during the Eleventh Five-Year Plan, the National Natural Science Foundation of China (Grant No. 40523006), the National Basic Research Program of China (“973” Project) (Grant No. 2006CB806305), and the Specialized Research Fund for State Key Laboratories