How do interplanetary shock impact angles control the size of the geoeffective magnetosphere?

In this paper, we investigate temporal and spatial magnetosphere response to the impact of interplanetary (IP) shocks with different inclinations and speeds on the Earth’s magnetosphere. A data set with more than 500 IP shocks is used to identify positive sudden impulse (SI⁺) events as expressed by the SuperMAG partial ring current index. The SI⁺ rise time (RT), defined as the time interval between compression onset and maximum SI⁺ signature, is obtained for each event. We use RT and a model suggested by Takeuchi et al. (2002) to calculate the geoeffective magnetospheric distance (GMD) in the shock propagation direction as a function of shock impact angle and speed for each event. GMD is a generalization of the geoeffective magnetosphere length (GML) suggested by Takeuchi et al. (2002), defined from the subsolar point along the X line toward the tail. We estimate statistical GMD and GML values which are then reported for the first time. We also show that, similarly to well-known results for RT, the highest correlation coefficient for the GMD and impact angle is found for shocks with high speeds and small impact angles, and the faster and more frontal the shock, the smaller the GMD. This result indicates that the magnetospheric response depends heavily on shock impact angle. With these results, we argue that the prediction and forecasting of space weather events, such as those caused by coronal mass ejections, will not be accurately accomplished if the disturbances’ angles of impact are not considered as an important parameter within model and observation scheme capabilities.     

天基微小空间碎片探测研究

随着空间碎片数量的不断增多,天基微小空间碎片探测已经成为一个热点．首先介绍了空间碎片在低地球轨道上的分布情况以及它对于航天器的危害,然后介绍了国外微小碎片探测器的基本情况,并在这些探测结果的基础上提出了一个探测器方案．这种探测器的传感器采用了新型的压电材料聚偏二氟乙稀(PVDF),使用了飞行时间法(TOF)准确测定空间碎片的飞行速度,以及快脉冲分析系统分析碎片的质量．     

铝颗粒云燃烧研究进展

为探究铝颗粒云燃烧特性,把握其研究进展,并为后续研究工作提供参考,本文首先简述了铝颗粒点火、燃烧过程,总结了铝颗粒燃烧机理;其次,综述了铝颗粒云燃烧的实验、理论和模拟研究进展,从不同维度分析了影响颗粒云火焰速度的关键参数,并提出颗粒云燃烧的研究方向,包括提升颗粒云燃烧实验颗粒分散均匀性与表征精度、降低火焰传播速度等实验结果散差、改善颗粒云燃烧理论预测模型精度及构建实用的颗粒云燃烧模拟CFD模型。     

Strong geomagnetic activity forecast by neural networks under dominant southern orientation of the interplanetary magnetic field

The paper deals with the relation of the southern orientation of the north–south component _Bz$B_z$ of the interplanetary magnetic field to geomagnetic activity (GA) and subsequently a method is suggested of using the found facts to forecast potentially dangerous high GA. We have found that on a day with very high GA hourly averages of _Bz$B_z$ with a negative sign occur at least 16 times in typical cases. Since it is very difficult to estimate the orientation of _Bz$B_z$ in the immediate vicinity of the Earth one day or even a few days in advance, we have suggested using a neural-network model, which assumes the worse of the possibilities to forecast the danger of high GA – the dominant southern orientation of the interplanetary magnetic field. The input quantities of the proposed model were information about X-ray flares, type II and IV radio bursts as well as information about coronal mass ejections (CME). In comparing the GA forecasts with observations, we obtain values of the Hanssen–Kuiper skill score ranging from 0.463 to 0.727, which are usual values for similar forecasts of space weather. The proposed model provides forecasts of potentially dangerous high geomagnetic activity should the interplanetary CME (ICME), the originator of geomagnetic storms, hit the Earth under the most unfavorable configuration of cosmic magnetic fields. We cannot know in advance whether the unfavorable configuration is going to occur or not; we just know that it will occur with the probability of 31%.     

A Prediction Method for△f0F2min of a Single Station From Interplanetary Parameters Based on Statistical Study

Using 86 CME-interplanetary shock events,the correlation between the peak values of （a） the solar wind parameters(B_z,E_y,P_dyn) and the geomagnetic indices（SYM-H,ASY-H,Kp）, （b） the coupling functions（Borovsky,Akasofu,Newell） and the geomagnetic indices,（c） the solar wind parameters/coupling functions/geomagnetic indices and the ionospheric parameter(Δf₀F_2min), are investigated.The statistical results show that in group（a）,B_{z min} and SYM-H_min have the best correlation,that in group（b）,the best correlation is between the peak values of Akasofu function (A_min) and SYM-H_min,and that in group（c）,the best correlation is between K_pmax andΔf₀F_2min. Based on the statistical results,a method for predicting f₀F₂ of a single station is attempted to be set up.The input is modified B_{z min} and the outputs are SYM-H_min andΔf₀F_2min.Then 25 CME-IPS events that caused geomagnetic storms in 1998 and 2009 are used to check the prediction method. The results show that our method can be used to predict SYM-H_min andΔf₀F_2min.     

基于T96模型的极尖区位形变化特性研究

基于T96模型,定义了极尖区的位形以及相关的描述参量(例如赤道向边界磁纬的最小值,纬向宽度,子午向和晨昏向的张角,倾斜度,扁平度,中心磁地方时等),讨论了太阳风动压(P_d)、行星际磁场(IMF)及磁暴强度对极尖区位形的影响.太阳风动压和磁暴强度越大,则极尖区的赤道向边界磁纬越小,纬向宽度越大,子午向和晨昏向的张角越大,倾斜度越大,扁平度越小;南向IMF B_z越强,则极尖区的赤道向边界磁纬越小,纬向宽度越小,子午向的张角越小,晨昏向的张角越大,倾斜度越大,扁平度越大;北向IMF B_z与南向IMF B_z的情况刚好相反;极尖区的中心磁地方时受IMF B_y控制,IMF B_y为正时,极尖区向昏侧移动,而IMF B_y为负时,极尖区则向晨侧移动,并且极尖区的中心磁地方时与IMF B_y之间有着良好的线性关系.将所得结果与前人的观测结果进行了简单比较,发现利用T96模型确定的极尖区位形与观测基本一致.     

月球巡视器太阳电池阵电性能仿真模型

建立精准的太阳电池阵电性能仿真模型,可为月球巡视器电源设计方案以及在轨任务规划的验证和优化提供保障。文章依据巡视器设计及月面环境的特殊性,建立了考虑遮挡、月尘等因素的太阳电池阵电性能仿真模型。该模型包括布阵文件编写及导入模块,光强、温度、老化影响计算模块,月尘影响计算模块,以及部分遮挡影响计算模块。对仿真模型进行了仿真分析,并将仿真结果与硬件实测值进行比较,结果表明:两者之间的误差可控制在5%以内,证明了模型的正确性和精准度。     

A stationary bow shock model for plasmas: The spherical blunt obstacle problem

We present an analytic model of a stationary bow shock which describes the interaction between a supermagnetosonic ambient wind and an obstacle with spherical-like frontal shape. We develop expressions for the bow shock’s geometry and the physical properties of the plasma sheath as functions of the upstream conditions. The solution is limited to magnetic fields parallel to the upstream velocity. The model allows to use any value of the upstream alfvenic and sonic Mach numbers and the polytropic index (γ$\gamma$), pointing out the influence of γ$\gamma$ for the magnetosheath compression and the bow shock shape. When both Mach numbers are small, the upstream magnetic field intensity affects also the bow shock shape. We compare our results with other models finding important consistencies. We also compare our results with in-situ data, we fund a reasonable qualitative agreement; however, it seems that our model underestimates the magnetosheath size.     

Pioneer 10 Doppler data analysis: Disentangling periodic and secular anomalies

This paper reports the results of an analysis of the Doppler tracking data of Pioneer probes which did show an anomalous behaviour. A software has been developed for the sake of performing a data analysis as independent as possible from that of Anderson et al. [Anderson, J., Laing, P.A., Lau, E.L., Liu, A.S., Nieto, M.M., Turyshev, S.G. Study of the anomalous acceleration of Pioneer 10 and 11. Phys. Rev. D 65, 082004, 2002], using the same data set. A first output of this new analysis is a confirmation of the existence of a secular anomaly with an amplitude about 0.8 nm s⁻² compatible with that reported by Anderson et al. A second output is the study of periodic variations of the anomaly, which we characterize as functions of the azimuthal angle φ$\phi$ defined by the directions Sun–Earth Antenna and Sun-Pioneer. An improved fit is obtained with periodic variations written as the sum of a secular acceleration and two sinusoids of the angles φ$\phi$ and 2φ$2\phi$. The tests which have been performed for assessing the robustness of these results are presented.