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401.
Ji Wu Weiying Sun Jianhua Zheng Cheng Zhang Hao Liu Jingye Yan Chi Wang Chuanbing Wang Shui Wang 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2011
Coronal mass ejections (CMEs) represent a great concentration of mass and energy input into the lower corona. They have come to be recognized as the major driver of physical conditions change in the Sun–Earth system. Consequently, observations of CMEs are important for understanding and ultimately predicting space weather conditions. This paper discusses a proposed mission, the Solar Polar Orbit Radio Telescope (SPORT) mission, which will observe the propagation of interplanetary CMEs to distances of near 0.35 AU from the Sun. The orbit of SPORT is an elliptical solar polar orbit. The inclination angle between the orbit and ecliptic plane should be about 90°. The main payload on board SPORT will be an imaging radiometer working at the meter wavelength band (radio telescope), which can follow the propagation of interplanetary CMEs. The images that are obtained by the radio telescope embody the brightness temperature of the objectives. Due to the very large size required for the antenna aperture of the radio telescope, we adopt interferometric imaging technology to reduce it. Interferometric imaging technology is based on indirect spatial frequency domain measurements plus Fourier transformation. The SPORT spacecraft will also be equipped with a set of optical and in situ measurement instruments such as a EUV solar telescope, a solar wind ion instrument, an energetic particle detector, a magnetometer, a wave detector and a solar radio burst spectrometer. 相似文献
402.
B. Nikutowski R. Brunner Ch. Erhardt St. Knecht G. Schmidtke 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2011
In the field of terrestrial climatology the continuous monitoring of the solar irradiance with highest possible accuracy is an important goal. SolACES as a part of the ESA mission SOLAR on the ISS is measuring the short-wavelength solar EUV irradiance from 16–150 nm. This data will be made available to the scientific community to investigate the impact of the solar irradiance variability on the Earth’s climate as well as the thermospheric/ionospheric interactions that are pursued in the TIGER program. Since the successful launch with the shuttle mission STS-122 on February 7th, 2008, SolACES initially recorded the low EUV irradiance during the extended solar activity minimum. Thereafter it has been observing the EUV irradiance during the increasing solar activity with enhanced intensity and changing spectral composition. SolACES consists of three grazing incidence planar grating spectrometers. In addition there are two three-signal ionisation chambers, each with exchangeable band-pass filters to determine the absolute EUV fluxes repeatedly during the mission. One important problem of space-borne instrumentation recording the solar EUV irradiance is the degradation of the spectrometer sensitivity. The two double ionisation chambers of SolACES, which could be re-filled with three different gases for each recording, allow the recalibration of the efficiencies of the three SolACES spectrometers from time to time. 相似文献
403.
研究柔性航天器的动力学与控制问题时,通常需要利用柔性附件的模态信息。为获取航天器的高精度姿态控制,必须解决柔性附件的振动抑制问题。配置压电传感/作动器是解决太阳翼振动控制的有效手段。针对基板表面粘贴压电传感/作动器的太阳翼,基于一阶剪切变形层板理论,建立了包含机电耦合效应对结构刚度贡献的有限元模型,并在连接机构等效梁单元中引入了轴向载荷。利用假设剪切应变方法解决了一阶剪切变形层板理论的剪切闭锁问题。仿真结果表明:太阳翼的动力学特征随压电传感/作动器配置方式的改变而改变;连接架轴向载荷可以大幅提高太阳翼的侧摆振动频率;给压电作动器施加控制电压可以增加太阳翼的结构阻尼。 相似文献
404.
利用WIND卫星的太阳风观测数据和地磁活动指数, 研究了太阳风扰动对环电流SYM-H指数, 西向极光电急流AL指数和东向极光电急流AU指数的影响. 结果表明, 太阳风动压增长和减少能够同步或延迟引起地磁活动指数的强烈扰动, 其包括环电流指数的上升, 西向极光电急流指数的下降和东向极光电急流指数的上升. 太阳风动压的突然剧烈增加还能够触发超级亚暴和大磁暴. 太阳风动压脉冲引起的地磁效应具有复杂的表现形式, 这说明太阳风动压脉冲的地磁效应不仅与太阳风动压脉冲大小和持续时间有关, 还与磁层本身所处的状态有关. 时间尺度较长, 消耗能量较大的磁暴只有大的持续时间较长的太阳风动压脉冲才能激发. 相似文献
405.
406.
407.
The direction of the sun is the easiest and most reliable observation vector for a solar sail running in deep space exploration. This paper presents a new method using only raw measurements of the sun direction vector to estimate angular velocity for a spinning solar sail. In cases with a con-stant spin angular velocity, the estimation equation is formed based on the kinematic model for the apparent motion of the sun direction vector;the least-squares solution is then easily calculated. A performance criterion is defined and used to analyze estimation accuracy. In cases with a variable spin angular velocity, the estimation equation is developed based on the kinematic model for the apparent motion of the sun direction vector and the attitude dynamics equation. Simulation results show that the proposed method can quickly yield high-precision angular velocity estimates that are insensitive to certain measurement noises and modeling errors. 相似文献
408.
ZHANG Heqi 《空间科学学报》2002,22(Z1)
In this paper main achievements in the area of space astronomy are summarized.During the flight of cosmic Gamma-Ray Burst Spectrometer(GRBS) onboard spacecraft Shenzhou-2(launched on 2001-01-10), much observational results of cosmic γ-ray burst and solar X, γ-ray burst are obtained. The preliminary analysis on space data has lead to some interesting results. Besides it, some other long-term space astronomy programs are briefly described here. 相似文献
409.
R. Esser 《Space Science Reviews》1994,70(1-2):331-340
Some of the main problems of solar wind expansion are addressed. Emphasis is placed on solar wind acceleration and the mass flux problem. It is demonstrated how these two properties of the flow depend on other plasma parameters such as temperature, density and helium abundance. The importance of placing constraints on a given solar wind flow in the inner corona and at larger distances from the sun simultaneously, is also shown. Whether and how these constraints can be derived from observations carried out by SOHO instruments is then discussed. 相似文献
410.
P. Veltri 《Space Science Reviews》1994,68(1-4):63-74
The possibility to perform in-situ measurements of velocity, magnetic field, density and temperature fluctuations in the Solar Wind has greatly improved our knoweledge of MHD turbulence not only from the point of view of space physics but also from the more general point of view of plasma physics.These fluctuations on the one hand extend over a wide range of frequencies (about 5 decades), a fact which seems to be the signature of turbulent non-linear energy cascade, on the other hand display, mainly in the trailing edge of high speed streams, a number of striking features: (i) a high degree of correlation between magnetic and velocity field fluctuations, (ii) a very low level of fluctuations in mass density and magnetic field intensity, (iii) a considerable anisotropy revealed by minimum variance analysis of the magnetic field correlation tensor. More recently it has been stressed that MHD turbulence in the Solar Wind displays a clear intermittent character.The picture which emerges from the most recent analytical theories and numerical simulations is presented. In particular the observations which give us informations about the dissipation mechanism, which remains yet largely unknown, are discussed. 相似文献