地球辐射带能量电子通量在不同地磁活动下的统计分析

利用大约15个月的CRRES卫星MEA能量电子观测数据,分别在地磁活动平静(0≤Kp)、中等(3≤Kp≤6)及强烈(6)的条件下,选取电子能量为148 keV, 509 keV, 1090 keV, 1581 keV的辐射带能量电子通量进行统计分析,得到了不同地磁活动条件下地球辐射带高能电子通量在(L, MLT)空间的全球分布模型.结果表明,在2的磁层区域,高能电子通量分布在不同的地磁活动指数Kp条件下差别明显;在12~18 MLT时段内高能电子的通量明显增大.     

Evolution of energetic electron fluxes at a geostationary orbit during solar cycles 22 and 23. 27-day variations

In this paper, we consider variations in energetic electron fluxes at a geostationary orbit, which are related to the Sun’s rotation period, during two solar cycles. We use data on energetic electron fluxes obtained from the GOES (1986–2007) (>2 MeV) and LANL (1996–2007) (50–225 and 315–1500 keV) satellites. Within the solar cycle, we observed both periods of high flux peak recurrence during several rotations and periods when there was no (or a low) 27-day recurrence. We show the similarity and difference between manifestations of flux recurrences from cycle to cycle. Insignificant manifestation of recurrence and its absence were observed mainly during the solar maximum. High electron flux recurrence was observed mainly at the phase of decline in solar activity (near the solar minimum). We show that for both solar cycles, there were several days (within the Bartels rotation) during which increased energetic electron fluxes would be most likely observed.     

利用地磁脉动预报地球同步轨道相对论电子通量的方法研究

本文利用低纬地磁台站的Pi1、Pi2地磁脉动（Pi1-2）资料和地球同步轨道的Pc5地磁脉动资料,对2004年1月到2006年12月38个磁暴事件的地磁脉动参数进行了统计分析.在此基础上,考虑相对论电子的局部加速机制,并加入损失机制,建立了一个初步的磁暴期间地球同步轨道相对论电子通量对数值的预报模型.利用该模型,我们对上述38个磁暴事件进行预报试验,最优化结果是：相对论电子通量对数值的预测值和观测值之间的线性相关系数为0.82,预报效率为0.67.这说明该模式具有较好的预报效果,也表明利用地磁脉动参数进行相对论电子通量预报是可行的.     

Effect of acceleration and loss rates on time variations in energetic electron fluxes during geomagnetic disturbances

The general properties of the effect of the acceleration and loss rate on the time variations in relativistic electron fluxes have been studied based on the analytical solutions to the nonstationary equation for the particle distribution function, taking into account diffusion in the momentum space (stochastic acceleration) and loss (due to particle escape from the acceleration region). The results of calculating the time variations in the fluxes of electrons with energies of 1 MeV are presented for different ratios of the loss-to-acceleration rates. The cases of instantaneous and prolonged injection of low-energy particles are considered. It has been proposed to estimate the acceleration and loss rate effectiveness based on the observed electron flux decrease rate at the end of the magnetic storm recovery phase.     

Prediction of maximal daily average values of relativistic electron fluxes in geostationary orbit during the magnetic storm recovery phase

The relation of the maximal daily average values of the relativistic electron fluxes with an energy higher than 2 MeV, obtained from the measurements on GOES geostationary satellites, during the recovery phase of magnetic storms to the solar wind parameters and magnetospheric activity indices has been considered. The parameters of Pc5 and Pi1 geomagnetic pulsations and the relativistic electron fluxes during the prestorm period and the main phase of magnetic storms have been used together with the traditional indices of geomagnetic activity (A _E, K _p, D _st). A simple model for predicting relativistic electron fluxes has been proposed for the first three days of the magnetic storm recovery phase. The predicted fluxes of the outer radiation belt relativistic electrons well correlate with the observed values (R ∼ 0.8–0.9).     

Indicators of an increase in the flux of relativistic electrons in geostationary orbit during geomagnetic storms

The relation of the fluxes of relativistic electrons in geostationary orbit during magnetic storms to the state of the magnetosphere and variations in the solar wind parameters is studied based on the GOES satellite data (1996–2000). It has been established that, in ～52–65% of all storms, the fluxes of electrons with energies higher than 0.6 and 2 MeV during the storm recovery phase are more than twice as high as the electron fluxes before a storm. It has been indicated that the probability of such cases is closely related to the prestorm level of fluxes and to a decrease in fluxes during the storm main phase. It has been found that the solar wind velocity on the day of the storm main phase and the geomagnetic activity indices at the beginning of the storm recovery phase are also among the best indicators of occurrence of storms with increased fluxes at the storm recovery phase.     

The behaviour of electron temperature under non-stationary conditions in dependence on geomagnetic latitude

Summary The electron temperature was monitored using a radiofrequency probe situated on the board of satellite INTERCOSMOS-8 from 30th Nov. to 25th Dec., 1972. All data were obtained under quiet geomagnetic conditions K_p<2⁺. The processing of data enabled us to compare the behaviour of the electron temperature T_e under non-stationary conditions of local sunrise and sunset for various geomagnetic latitudes. The results showed a different behaviour of the electron temperature in mid-latitudes and in the region of the magnetic equator in dependence on angle x.     

同步轨道相对论电子通量长期倒空事件的统计研究

地球辐射带中有"杀手"电子之称的相对论电子通量增强和损失过程一直是空间物理学和空间天气学研究的热点.本文通过对2000—2016年间,地球同步轨道相对论电子通量降低至背景通量水平并持续时间长达3天以上这一特殊现象进行了相关统计研究.从事件的时间分布角度,本文研究了约1.5个太阳活动周内共62例事件随太阳活动水平高低的分布情况,结果表明:在太阳活动周下降期有较少的事件发生,而在峰年、谷年这类事件的发生率与太阳活动水平的高低并没有直接联系.随后,我们对这62例事件在开始、持续、结束三个阶段分别做了一些相关参数的统计,探讨相对论电子通量长期倒空事件的客观规律和产生机制.研究结果表明:事件发生前,太阳风动压、密度的显著增加引起磁层顶向内收缩,等离子体层顶一直维持在高L区域,IMF B_z分量南向和磁暴过程使相对论电子通量通过绝热和非绝热等物理损失机制降至背景通量水平.当这些相对论电子达到背景通量水平后,较弱的太阳风条件和地磁活动水平不足以提供充分的可以使相对论电子通量增长的源;虽然有些相对论电子通量长期倒空事件期间存在中、小磁暴过程,但这些强度较弱的磁暴很可能不会显著地影响...     

Comparison of the electron density variations measured with instruments of the ISZF SO RAN radar complex under the conditions of different geomagnetic disturbance

The variations in the electron density measured with the incoherent scatter radar, DPS-4 digisonde, and FMCW ionosonde are compared in this work. The main regularities in differences are explained by the effect of different-scale ionospheric irregularities. Considerable morning gradients of electron density result in that ionosondes give increased values as compared to the incoherent scatter radar data. Electron density disturbances measured with different instruments can be of correlated and uncorrelated character. Uncorrelated disturbances are explained by intense medium-scale ionospheric irregularities. Correlated disturbances are caused by large-scale irregularities. Observation of such disturbances can be used to determine the velocity and direction of a disturbance.     

Strong localized variations of the low-altitude energetic electron fluxes in the evening sector near the plasmapause

Specific type of energetic electron precipitation accompanied by a sharp increase in trapped energetic electron flux are found in the data obtained from low-altitude NOAA satellites. These strongly localized variations of the trapped and precipitated energetic electron flux have been observed in the evening sector near the plasmapause during recovery phase of magnetic storms. Statistical characteristics of these structures as well as the results of comparison with proton precipitation are described. We demonstrate the spatial coincidence of localized electron precipitation with cold plasma gradient and whistler wave intensification measured on board the DE-1 and Aureol-3 satellites. A simultaneous localized sharp increase in both trapped and precipitating electron flux could be a result of significant pitch-angle isotropization of drifting electrons due to their interaction via cyclotron instability with the region of sharp increase in background plasma density.     

Chaotic behaviour of interplanetary magnetic field under various geomagnetic conditions

In the present study, the deterministic chaotic behaviour of interplanetary magnetic field (IMF) under various geomagnetic conditions of low and high solar active periods was analyzed, using the time series of IMF |B| and B_z, by employing chaotic quantifiers like, Lyapunov exponent, Tsallis entropy, correlation dimension, and non-linear prediction error. We have investigated whether the chaotic behaviour of interplanetary magnetic field would modify, when it produces major geomagnetic storms, and how it depends on the phase of solar activity. The yearly average values of Lyapunov exponent for the time series of IMF |B| and B_z, show solar flux dependence, whereas those values of entropy, correlation dimension and non-linear prediction error had no significant solar flux dependence. The yearly average values of entropy for quiet periods are higher compared to those values for major storm periods belonging to low/high solar active conditions, for both the time series |B| and B_z.     

Interpretation of the energy spectrum and time dynamics of electron fluxes with energies of 0.8–6.0 MeV in geostationary orbit during the recovery phase of the magnetic storm of April 6, 2000

The electron energy spectrum in the energy range of 0.8–6.0 MeV and the time dynamics of electron fluxes during the prolonged (～10 days) recovery phase of the magnetic storm of April 6, 2000, have been analyzed using the Express-A2 geostationary satellite data. These data have been interpreted based on the analytical solution to the nonstationary equation for the particle distribution function taking into account statistical acceleration and catastrophic particle escape from the acceleration region.     

不同太阳活动及地磁条件下的电导率分布变化

电离层电导率在不同的太阳活动和地磁条件下会发生变化. 本文通过中性大气经验模式NRLMSISE_00（Neutral Atmosphere Empirical Model_2000,简称NRLMSISE_00）和电离层经验模式IRI_2001（International Reference Ionosphere_2001,简称IRI_2001）计算电离层的电子、离子碰撞频率以及电导率,并简要讨论了120 km和300 km高度上的电导率在不同季节、不同太阳活动和地磁指数下的经纬分布. 结果显示,电导率的分布与日照密切相关,且随太阳活动的变化而变化. 磁暴时电导率随地磁活动的变化相对于随太阳活动的变化要小,在120?km高度,磁暴期间电导率在低纬地区和高纬地区发生不同变化,且Pedersen电导率和Hall电导率变化趋势相反,向两极靠近,电导率变化幅度略有增长;在300?km高度上,磁暴对低纬地区和高纬地区电导率的影响要比120?km处大,Pedersen电导率和Hall电导率变化趋势相同,且越向两极靠近电导率的变化幅度越大.     

Climatology of total electron content near the dip equator under geomagnetic quiet-conditions

This study analyzes the TEC data during 1998–2007, observed by the AREQ (16.5°S, 71.5°W) GPS station to investigate the equatorial ionospheric variations under geomagnetic quiet-conditions. The diurnal TEC values generally have a maximum value between 1330 and 1500 LT and a minimum around 0500 LT. For the seasonal variation, the semi-annual variation apparently exists in the daytime TEC with two peaks in equinoctial months. In contrast, this semi-annual variation is not found in the nighttime. Furthermore, the results of the annual variation show that the correlation between the daytime TEC value and the solar activity factor is highly positive.     

Parameters of the near-earth interplanetary medium under quiet and disturbed geomagnetic conditions

The distributions of the parameters of the solar wind, IMF, and physical fields (E _y component of the SW electric field, compression field DCF) and the rms errors (σ) of measurements, depending on the daily characteristic of geomagnetic disturbance (Cp), are considered. The scatter of parameters in the interplanetary medium (IM) is actually considerable even during a long interval of geomagnetic quiet. It has been indicated that an unambiguous correspondence between the IM parameters and the characteristic of geomagnetic activity on the Earth is absent, and we have only tendencies toward an increase (decrease) in the parameter of the near-Earth medium (physical quantity) with increasing geomagnetic activity. These tendencies are transformed into linear relationships only after the three-fold averaging of values (hourly, daily, annual), which corresponds to numerous equations of relation between IM parameters and different geomagnetic indices, obtained by many researchers based on statistical analyses.     

Response of the electron density profiles to geomagnetic disturbances in January 2005

Studia Geophysica et Geodaetica - The ionospheric response to geomagnetic storms is usually investigated by considering the variability of the critical frequency of the F2-layer (foF2) or the total...     

高能电子爆发与绕月卫星表面电位大幅下降的联动效应

“嫦娥”一号、二号绕月飞行经历地球磁尾边界层区域时,分别在2007年11月26日-2008年2月5日和2010年10月3日-2011年2月28日,发现了15次月球轨道0.1~2 MeV电子急剧增加（Bursts of 0.1~2 MeV Energetic Electrons,BEE）,卫星周围等离子体离子加速的现象.统计研究表明,这类现象发生在稳定太阳风和弱行星际磁场条件下,且无显著空间环境扰动事件发生时,离子的加速滞后于高能电子爆发,离子能量的变化与高能电子通量的时间演化正相关,地球磁鞘内侧或边界层过渡区域是该类现象的高发区,离子能量增加时卫星表面电位大幅下降可达负几千伏.为了研究高能电子爆发与绕月卫星表面电位变化的关系及其对月球表面电位的影响,本文用电流平衡法建立绕月卫星和月球表面充电模型,并假设能量电子（>2 eV~2 MeV）满足幂律谱的分布,模拟急剧增加的能量电子对卫星和月球表面电位的影响.模拟结果表明,能量电子急剧增加使得绕月卫星和月球表面电位大幅下降;能量电子总流量>1011 cm-2时,绕月卫星和月球表面充电电位可达负上千伏;月球充电到大的负电位的时间仅为卫星充电时间的1/10.鉴于高能电子急剧增加事件的高发生率（~125次/年）,能量电子急剧增加使得绕月卫星表面电位大幅下降的发生率应大于实测等离子体离子加速现象的发生率（~25次/年）.     

Diurnal variations of the total electron content under quiet helio-geomagnetic conditions

The morphology of averaged diurnal variations of total electron content (TEC) under quiet helio-geomagnetic conditions for all latitudinal bands and various longitudes has been studied using Global Ionospheric Maps (GIMs) datasets. The diurnal TEC variation maximum is generally registered at 14–15 LT. The maximum is 38±5, 14±2, 10±2 TECU (TECU is generally accepted TEC unit) at the equatorial, middle and high latitudes. The nighttime TEC minimum is within 5–7 TECU regardless of a season, latitude and longitude. At the equatorial latitudes TEC exhibits the most significant daily/season variations and the asymmetry of its behavior in the hemispheres near the equinox. Abnormal diurnal TEC variations (evening maximum, near-noon minimum) are observed at middle and high latitudes in summer due to atmospheric wind effects. The comparison of the averaged diurnal TEC variations with the behavior of the ionospheric F2-layer critical frequency indicated that GIMs describe daily/annual TEC variations reasonably well.     

Cracking conditions of crude oil under different geological environments

There are mainly 3 kinds of existing states of oil generating from source rocks, that is, dispersive liquid hydrocarbon inside of source rock, dispersive liquid hydrocarbon outside of source rock and concentrated liquid hydrocarbon outside of source rock. Because of the differences in thermal history and medium conditions around, and the interaction of organic and inorganic matter, the liquid hydrocarbon with 3 kinds of existing state has different cracking conditions. The gas generation dynamics experiments of crude oil matching different mediums indicate that the distribution of activation energy of methane changes a lot according to medium difference. The carbonate has a main influence on oil cracking conditions and can largely reduce its activation energy, which reflects the lower cracking temperature of crude oil. The mudstone takes a second place and the sandstone is the smallest. The catalytic cracking function to the oil of the carbonate, of the mudstone and of the sandstone changes weaken in turn. The corresponding R _o values of main gas generation period in different mediums are as follows: 1.5%–3.8% with pure crude oil, 1.2%–3.2% with dispersive crude oil in carbonate, 1.3%～3.4% with dispersive crude oil in mudstone and 1.4%–3.6% with dispersive crude oil in sandstone. The influence of pressure to crude oil cracking is relatively complicated. In the low heating speed condition, pressure restrains the oil cracking and gas generation, but in the high heating speed condition, pressure has an indistinctive influence to the oil cracking and gas generation. Pressure also makes a different effort in different evolvement stage. Taking the middle and lower Cambrian source rocks in the Tarim Basin as an example, primary oil generating quantity is 2232.24×10⁸t, residual oil and oil cracking gas quantity is 806.21×10⁸t and 106.95×10¹²m³ respectively.