Investigation of CME properties using the data of SDO and PROBA2 spacecraft

Formation and motion (at the initial stage) of six limb CMEs detected in the period June 2010 to June 2011 are investigated using the high-resolution data of the PROBA2 and SDO spacecraft combined with the data of SOHO/LASCO coronagraphs. It is demonstrated that several loop-like structures of enhanced brightness originate in the region of CME formation, and they move one after another with, as a rule, different velocities. These loop-like structures in the final analysis form the frontal structure of CME. Time dependences of the velocity and acceleration of the ejection’s front are obtained for all CMEs under consideration. A conclusion is drawn about possible existence of two classes of CMEs depending on their velocity time profiles. Ejections, whose velocity after reaching its maximum sharply drops by a value of more than 100 km/s and then goes over into a regime of slow change, belong to the first class. Another class of CMEs is formed by ejections whose velocity changes slowly immediately after reaching the maximum. It is demonstrated that the CME’s angular dimension increases at the initial stage of ejection motion up to a factor of 3 with a time scale of doubling the angular size value within the limits 3.5–11 min since the moment of the first measurement of this parameter of an ejection. For three CMEs it is shown that at the initial stage of their motion for a certain time interval they are stronger expanded than grow in the longitude direction.     

空间等离子体环境中的高能带电粒子加速机制

空间环境中充满能量从几十keV到几MeV的高能带电粒子,这些粒子可导致在轨航天器表面和内部带电甚至单粒子效应,从而引发航天器故障。高能粒子的产生和日地空间环境中的爆发现象如耀斑、磁层亚暴等密切相关。文章综述了与这些爆发现象相关的磁重联、激波和等离子体波动等加速带电粒子的物理过程。     

Coronal mass ejection (CME) activity of low mass M stars as an important factor for the habitability of terrestrial exoplanets. I. CME impact on expected magnetospheres of Earth-like exoplanets in close-in habitable zones

Low mass M- and K-type stars are much more numerous in the solar neighborhood than solar-like G-type stars. Therefore, some of them may appear as interesting candidates for the target star lists of terrestrial exoplanet (i.e., planets with mass, radius, and internal parameters identical to Earth) search programs like Darwin (ESA) or the Terrestrial Planet Finder Coronagraph/Inferometer (NASA). The higher level of stellar activity of low mass M stars, as compared to solar-like G stars, as well as the closer orbital distances of their habitable zones (HZs), means that terrestrial-type exoplanets within HZs of these stars are more influenced by stellar activity than one would expect for a planet in an HZ of a solar-like star. Here we examine the influences of stellar coronal mass ejection (CME) activity on planetary environments and the role CMEs may play in the definition of habitability criterion for the terrestrial type exoplanets near M stars. We pay attention to the fact that exoplanets within HZs that are in close proximity to low mass M stars may become tidally locked, which, in turn, can result in relatively weak intrinsic planetary magnetic moments. Taking into account existing observational data and models that involve the Sun and related hypothetical parameters of extrasolar CMEs (density, velocity, size, and occurrence rate), we show that Earth-like exoplanets within close-in HZs should experience a continuous CME exposure over long periods of time. This fact, together with small magnetic moments of tidally locked exoplanets, may result in little or no magnetospheric protection of planetary atmospheres from a dense flow of CME plasma. Magnetospheric standoff distances of weakly magnetized Earth-like exoplanets at orbital distances 相似文献   

Statistical Relationships between Solar, Interplanetary, and Geomagnetic Disturbances, 1976–2000: 2

In this paper we continue the analysis of the influence of solar and interplanetary events on magnetospheric storms that was started in [1]. Two data sets are additionally analyzed in the present study: solar flares of importance M5 and greater in 1976–2000 and halo CMEs observed by the SOHO spacecraft during the period of 1996–2000. It is demonstrated that the statistical characteristics of the new set of flares and of that analyzed before in [1] differ little, while the geoeffectiveness of the halo CMEs turned out to be much less than that of the previously published CMEs.     

Statistical Relationships between Solar,Interplanetary, and Geomagnetic Disturbances, 1976–2000: 3

In this paper we continue the analysis of the influence of solar and interplanetary events on magnetic storms of the Earth that was started in [9, 10]. Different experimental results on solar-terrestrial physics are analyzed in the study and the effects are determined that arise due to differences in the methods used to analyze the data. The classifications of magnetic storms by the K _p and D _st indices, the solar flare classifications by optical and X-ray observations, and the classifications of different geoeffective interplanetary events are compared and discussed. It is demonstrated that quantitative estimations of the relationships between two types of events often depend on the direction in which the events are compared. In particular, it was demonstrated that the geoeffectiveness of halo CMEs (that is, the percentage of Earth-directed coronal mass ejections that result in geomagnetic storms) is 40–50%. Higher values given in some papers were obtained by another method, in which they were defined as the probability of finding candidates for a source of geomagnetic storms among CMEs, and, strictly speaking, these values are not true estimates of the geoeffectiveness. The latter results are also in contrast with the results of the two-stage tracing of the events: first a storm—an interplanetary disturbance, and then an interplanetary disturbance—a CME.     

Space-time structure of ion-cyclotron waves in the topside ionosphere as observed onboard the <Emphasis Type="Italic">ST</Emphasis>-<Emphasis Type="Italic">5</Emphasis> satellites

Results of observations of ion-cyclotron (IC) waves onboard the ST-5 satellites in the topside ionosphere (heights from a few hundred up to thousands of km) are presented. In this project, three identical micro-satellites were located during three months in 2006 in almost identical orbits with distances between them from first thousands to hundreds of km. All ion-cyclotron wave packets detected by two-three probes were observed at crossing one and the same latitude, which manifests their narrow localization in latitude with a characteristic scale from the first tens to 100 km. In no event IC waves were recorded with comparable amplitudes by all three satellites. At the same time, in the case of ST-5 flight near the ground-based induction magnetometer, a long emission in the same frequency range on the ground corresponded to a burst of IC waves in the topside ionosphere. This can indicate to the fact that an IC instability develops not continuously, but in the pulsing regime with a characteristic time of up to ∼10 min. A change in the rotation direction when a satellite crosses the wave structure is a characteristic feature of the polarization structure of registered transverse waves. The detected effects are discussed from the point of view of the existing models of generation and waveguide propagation of IC waves.     

纬度未知条件下捷联惯导系统初始对准分析

在捷联惯导系统静基座初始对准的传统方法中,一般要求准确知道当地的地理纬度,如果给定的纬度存在误差,将可能影响初始对准精度。在静基座条件下并且地理纬度未知时,研究捷联惯导系统的初始对准实现问题,并对初始对准精度作详细分析。研究结果表明,在静基座条件下,借助于捷联惯组中的陀螺和加速度计的测量值可以估计出对准点处的地理纬度,再利用估计纬度进行初始对准,如果选择初始对准算法适当,纬度估计误差将不会影响对准精度。     

利用低轨道卫星间微波信号探测反演温湿廓线

通过同时测量微波信号的折射和吸收信息,低地球轨道卫星间（LEO-LEO）微波掩星探测技术能够独立反演温度和水汽廓线。通过仿真手段,首先,正演模拟了微波信号穿过大气层后由折射和吸收效应分别导致的相位延迟和振幅衰减,在此基础上,对温度、水汽和云中液态水反演廓线进行了个例分析,然后,统计分析了温度和水汽在不同纬度带的反演性能,以及云对反演精度的影响。结果表明：温度在约35 km以上存在明显正偏差,高纬度的最大,中纬度次之,低纬度最小。水汽反演误差在约4 km以下明显增大,低纬度的最大,中纬度次之,高纬度最小。有云存在时,需要去除云的吸收作用,否则温度和水汽会出现明显的正偏差。上述研究为进一步发展LEO-LEO掩星探测计划提供了理论参考依据。     

Coronal mass ejections in July 2005 and an unusual heliospheric event

Using the events in July 2005 as an example, the causes and peculiarities of Forbush effects produced by solar sources remote from the central zone are discussed. The event in question differs from other effects observed at the periphery of interplanetary disturbances by strong variations in cosmic rays on the background of weak disturbances in the solar wind and magnetic field of the Earth. The cloud of magnetized plasma ejected from the Sun was large and fast, but it passed to the west from the Sun-Earth line. According to performed estimates, the mass of the ejected substance was close to the upper boundary of mass for coronal mass ejections (CMEs). Anomalous parameters and high modulation capability of the formed solar wind disturbance are explained, in particular, by the fact that it combined several CMEs and that the last fast disturbance was prepared by a series of impulsive events in the active region of the Sun. Usually, such a great mass is ejected directly after the main energy release in strong solar flares. In the given case, a powerful MHD disturbance occurred approximately half an hour after a maximum of hard X-ray burst under the conditions when gas pressure in the flare loops became close to magnetic pressure, which was just a premise of the largescale ejection.     

Localized Enhancements of Energetic Proton Fluxes at Low Altitudes in the Subauroral Region and Their Relation to the Pc1 Pulsations

A special kind of variation of energetic proton fluxes inside the anisotropic precipitation zone is considered using the data from the low-altitude satellites NOAA/TIROS. The variation is characterized by a localized (within 1° of latitude) enhancement of >30 keV protons, both trapped at the spacecraft altitude and precipitating. A close correlation is shown between the morphological characteristics of the proton precipitation and the Pc1 pulsations observed by the ground-based geophysical observatory Sodankylä. The probability of observation of the Pc1 pulsation by a ground-based station decreases with increasing MLT distance between this station and the projection of the satellite detecting the precipitating protons. The Pc1 pulsation frequency decreases as the proton burst latitude increases. These findings support the ion-cyclotron mechanism of the Pc1 production suggesting that both wave generation and particle scattering occur in the source region.     

The Shuttle Radar Topography Mission (SRTM): a breakthrough in remote sensing of topography

The Shuttle Radar Topography Mission (SRTM), flown on the Space Shuttle Endeavour on Flight STS-99 and launched on 11 February 2000, will produce digital elevation data of the Earth's land mass between 60 degrees north latitude and 54 degrees south latitude. This data will be at least one order of magnitude more precise in the elevation resolution, and will have postings of 30 m, representing an order of magnitude increase in the density of the postings over currently available data.     

Impact of helio-and geophysical disturbances on thermobaric and climatic characteristics of the Earth’s troposphere

We present the mechanism and the concept of a model of the solar activity impact on thermobaric and climatic characteristics of the troposphere. Both are based on the idea of parametric action. The results of analysis are presented concerning specific features and regularities of changes in temperature regime of the troposphere in the period of variable helio-and geophysical activity, as well as long-term variations of temperature and heat content of the troposphere. The influence of changes in circulation in the atmosphere and ocean on processes in the system atmosphere-ocean-cryosphere is considered: thermohaline circulation of the oceans and energy exchange between the atmosphere and ocean. The revealed regularities find their complete explanation within the context of a model and mechanism of solar activity impact on climatic characteristics of the troposphere that were suggested previously by the authors.     

Sporadic plasma streams and their sources in the period of extraordinary solar activity from October 26 to November 6, 2003

Based on the results of investigations made by various authors applying different semiempirical models, we have formulated the principles of a complex method that allows one to associate sporadic streams of the solar wind (SW) at the Earths orbit with coronal mass ejections (CMEs), which are their sources on the Sun. This method is applied to an analysis of the events in the interval from October 26 to November 6, 2003. It is shown that, in the period under consideration, which is close to the maximum of solar activity, the majority of CMEs (up to 80% of their total number) turn out to be at the base of a chain of streamers. It is also shown that the component of the interplanetary magnetic field is the main factor of geoeffectiveness for six sporadic SW streams. At the same time, an unusually low value of the index minD_st< -300 nT for two streams with the velocities V_max > 1000 km/s is a consequence of the fact that they are not isolated; i.e., the subsequent stream moves through the medium disturbed by the preceding stream.Translated from Kosmicheskie Issledovaniya, Vol. 42, No. 6, 2004, pp. 595–607.Original Russian Text Copyright © 2004 by M. Eselevich, V. Eselevich.     

Methods of Separating an Adiabatic Component in Storm-Associated Flux Variations of the Ion Ring Current

On the basis of an invariant representation of ion spectra with > 0.1 keV/nT, new methods of separation and quantitative analysis of the adiabatic component of storm-associated variations of fluxes of ions in the geomagnetic trap from the satellite data are developed. The regularities of adiabatic variations of flux ratios for different ion components, associated with their spectra scaling laws, are considered.     

地球边缘大气密度时空特性分析

分析了地球边缘大气密度的时变特性及空间分布特性。从物理原因出发并基于NRLMSISE-00和MET-99大气模型计算随不同时空变量变化的相对大气密度,以说明各时空因素对地球边缘大气密度的影响程度。分析结果表明地球边缘大气密度具有较强的时变特性,昼夜和季节均对大气密度产生一定影响。空间特性表现为纬度对大气密度的影响明显,而经度影响微弱。季节不同导致纬度的影响程度不同,纬度因素在夏季和冬季的影响强于春秋。随着纬度的增加,季节对地球边缘大气密度的影响逐渐增强,而当地时间的影响呈减弱趋势。相比较而言,低纬区的昼夜波动强于季节波动,高纬区的季节波动强于昼夜波动。     

Identification of coronal sources of the solar wind from solar images in the EUV spectral range

Methods of localizing coronal sources of the solar wind (SW), such as coronal holes, quasi-stationary fluxes from active regions, and transient sources associated with small-scale active phenomena are considered based on vacuum-ultraviolet (EUV) images of the corona at low solar activity during the initial period of the 24th solar cycle (2010). It is shown that a SW velocity profile can be calculated from the relative areas of coronal holes (CH) at the central part of the disk based on the images in the ranges of 193 and 171 Å. The images in the 193 Å describe the geometry of large HCs that represent sources of fast SW well. The images in 171 Å are a better visualization of small CHs, based on which the profile of a slow SW component was calculated to a high accuracy (up to 65 km/s). According to Hinode/EIS data of October 15, 2010, using the Doppler spectroscopy method at the streamer base over the active region 11112, the source of the outgoing plasma flux with the mean velocity of 17 km/s was localized in the magnetic field region with an intensity of less than 200 Gauss. According to the estimate, the density of the plasma flux from this source is an order of magnitude greater than the value required for explaining the distinction between the calculated and measured profiles of a slow SW velocity. For finding the transient SW component based on small-scale flare activity, SW parameters were analyzed for the periods of flares accompanied by coronal mass ejections (CMEs), and for the periods without flares, according to the data obtained in 2010 from the ACE and GOES satellites and by coronagraphs on the STEREO-A and -B spacecraft. The ion ratios C⁺⁶/C⁺⁵ and O⁺⁷/O⁺⁶ and the mean charge of Fe ions for periods with flares were shown to be shifted toward large values, suggesting the presence of a hot SW component associated with flare activity. A noticeable correlation between the maximum charge of Fe ions and the peak power of a flare, previously observed for flares of a higher class, was confirmed. The mean value of the SW flux density during the periods of flares was 30% higher than that in the periods without flares, which is possibly associated also with the growth of fluxes from other sources with an increasing solar activity level. Based on the example of a series of flares of October 13–14, 2010, it was supposed that transient SW fluxes from the weak flares at low solar activity can manifest themselves in the form of interplanetary ICME-transients.     

一种易于硬件实现的CCSDS图像数据压缩算法

文章提出了一种易于硬件实现的CCSDS图像数据无损压缩算法。图像数据经过小波变换后,统计规律不尽相同。为了有效进行数据压缩,该标准针对不同的统计规律,采用不同的熵编码。针对不同的图像,讨论了直流系数（DC）量化编码和块交流系数比特深度编码中的参数k、熵编码中长度为3比特码字的编码方式参数choicel和choice3以及长度为4比特码字的编码方式参数choice2和choice4等参数的最优化选择。仿真结果表明,该算法有较低复杂度,易于硬件实现,而且能够有效优化。使输出码率最短。     

夜气辉对天基光学碎片探测的影响分析

设计并完成了夜气辉背景下的天基碎片观测试验，获取了综合谱段的观测数据。基于观测数据进行夜气辉的辐射特性及其对天基碎片探测的影响分析。结果表明，夜气辉辐射随纬度和高度呈现一定的分布特点，这些特点均符合夜气辉的理论分布规律。在约90 km处辐射最强，亮度可达到单位积分时间每平方角秒近15星等，这对恒星及碎片提取概率影响较大，其中，13等星的提取概率仅为40.5%。     

SAA域选划对天基探测卫星影响简析

通过仿真计算南大西洋异常区(SAA)高能粒子的通量与能量,分析不同通量阈值与能量阈值对SAA空间分布的影响,并以科学实验卫星为研究对象,对其历经SAA的时间百分比进行连续24 h和6个月的统计,获得了SAA对卫星常规运行的工作时间影响。结果表明:在50 MeV能量阈值条件下,500 cm~(-2)?s~(-1)较100 cm~(-2)?s~(-1)通量阈值对SAA空间分布的影响范围在纬度上相差约23.35%,经度上相差约27.06%,历经SAA时间上缩短约48.0%;在100 cm~(-2)?s~(-1)通量阈值条件下,150 MeV较50 MeV能量阈值对SAA空间分布的影响范围在纬度上相差约13.86%,经度上相差约17.29%,历经SAA时间上缩短约31.7%。     

星载合成孔径雷达回波多普勒频率的计算

从星载合成孔径雷达（ＳＡＲ）与目标的相对运动关系出发，以ＳＡＲ发射信号的波长、卫星的轨道参数和目标的位置（地心经纬度）为已知条件，导出了计算目标回小以的多普勒频率的解析公式，这对于星载ＳＡＲ系统的性能 初步设计具有重要作用。