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1.
对目前太阳能的几种常见的应用领域及相关装置进行了分析和研究,并在此基础上,结合相关理论,设计了利用太阳能的新型装置,如:太阳能房、太阳能热发电装置、聚光式太阳能电池发电装置等,这些装置将为更好地利用太阳能开辟新的途径.太阳能作为一种新兴的可再生能源有着不可限量的发展前景. 相似文献
2.
Three ways of the energy transfer in the Earth's magnetosphere are studied. The solar wind MHD generator is an unique energy
source for all magnetospheric processes. Field-aligned currents directly transport the energy and momentum of the solar wind
plasma to the Earth's ionosphere. The magnetospheric lobe and plasma sheet convection generated by the solar wind is another
magnetospheric energy source. Plasma sheet particles and cold ionospheric polar wind ions are accelerated by convection electric
field. After energetic particle precipitation into the upper atmosphere the solar wind energy is transferred into the ionosphere
and atmosphere. This way of the energy transfer can include the tail lobe magnetic field energy storage connected with the
increase of the tail current during the southward IMF. After that the magnetospheric substorm occurs. The model calculations
of the magnetospheric energy give possibility to determine the ground state of the magnetosphere, and to calculate relative
contributions of the tail current, ring current and field-aligned currents to the magnetospheric energy. The magnetospheric
substorms and storms manifest that the permanent solar wind energy transfer ways are not enough for the covering of the solar
wind energy input into the magnetosphere. Nonlinear explosive processes are necessary for the energy transmission into the
ionosphere and atmosphere. For understanding a relation between substorm and storm it is necessary to take into account that
they are the concurrent energy transferring ways.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
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Jingxiu Wang 《Space Science Reviews》2001,95(1-2):55-65
Transient solar activities are defined in this paper as explosive releases of magnetic energy in the solar atmosphere. By photospheric driving we mean, in this paper, the roles played by the processes observed in the photosphere in accumulating the magnetic energy and complexity in the solar atmosphere. We have tried to clarify the key elements of the driving processes, based on both theoretical considerations and observations. 相似文献
6.
针对太阳能无人机在飞行状态下可能出现的太阳能电池局部遮挡情况,开展相应的太阳能电池最大功率点追踪算法和能源控制研究。通过将发光亮度引入相对吸引力计算过程对萤火虫算法进行改进,实现了局部阴影情况下太阳能电池最大功率点的高效追踪。以此为基础,设计了考虑局部遮挡情况下太阳能无人机的太阳能电池/蓄电池混合能源状态机控制规则。以"蒲公英I"无人机为例,建立了太阳能电池阵列模型,开展了考虑局部遮挡情况下太阳能电池最大功率点追踪仿真实验;基于"蒲公英I"飞行剖面,开展了考虑局部遮挡情况的混合能源控制仿真试验。研究结果表明:改进的萤火虫算法可以实现在局部阴影情况下太阳能电池最大功率点的有效跟踪,与萤火虫算法相比收敛时间更短、且功率波动幅度更小;采用改进萤火虫算法和状态机能源管理策略,在考虑局部遮挡的飞行状态下可以实现太阳能电池/蓄电池之间的合理功率分配与控制。 相似文献
7.
The basics of performing the initial electrical power subsystem (EPS) sizing for a spacecraft using solar cells for an energy source and batteries for energy storage are covered. The basic engineering inputs are described. The outputs are the first estimate of the number of solar cells, the solar array area, and the number of batteries required. A spreadsheet program to keep track of the inputs, perform the calculations, and document the inputs and outputs was written 相似文献
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Tatsuzo Obayashi 《Space Science Reviews》1964,3(1):79-108
A review is given of the features of solar particle emissions which cause various terrestrial disturbances. Three types of corpuscular emissions, namely, solar cosmic rays, energetic storm protons and plasma clouds, are associated with intense solar flares. Outward streaming of the solar wind and of beams of enhanced activity originate from the quiescent solar corona. It is shown that these solar particles propagate through interplanetary space, being modulated in a systematic way by existing magnetic fields. Time variations of solar flare particle flux, and their energy spectrum, are discussed. 相似文献
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Steven R. Cranmer 《Space Science Reviews》2012,172(1-4):145-156
The origins of the hot solar corona and the supersonically expanding solar wind are still the subject of much debate. This paper summarizes some of the essential ingredients of realistic and self-consistent models of solar wind acceleration. It also outlines the major issues in the recent debate over what physical processes dominate the mass, momentum, and energy balance in the accelerating wind. A key obstacle in the way of producing realistic simulations of the Sun-heliosphere system is the lack of a physically motivated way of specifying the coronal heating rate. Recent models that assume the energy comes from Alfvén waves that are partially reflected, and then dissipated by magnetohydrodynamic turbulence, have been found to reproduce many of the observed features of the solar wind. This paper discusses results from these models, including detailed comparisons with measured plasma properties as a function of solar wind speed. Some suggestions are also given for future work that could answer the many remaining questions about coronal heating and solar wind acceleration. 相似文献
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The understanding of the relative intensity variations in cosmic ray ions and electrons with respect to solar modulation is a grand challenge for cosmic ray modulation theory. Although effects of the heliospheric neutral sheet, gradient-curvature drifts, and merged interaction regions provide qualitative explanations for observed solar cycle variations of high energy protons and ions, these effects do not account for the anomalously high intensities of high energy galactic electrons at 22-year intervals of the solar magnetic solar cycle. From the similar modulation responses of protons and heavy ions it does not appear that cosmic ray pressure effects, dominated by protons, can account for the chargesign asymmetry of cosmic ray modulation. External factors including modulation in the heliosheath and polar linkage to the interstellar magnetic field are examined as potential causes of symmetry breaking for electron modulation with respect to the solar magnetic polarity at solar minimum. 相似文献
13.
Flight trajectory optimization of sun-tracking solar aircraft under the constraint of mission region
《中国航空学报》2021,34(11):140-153
The optimal yawing angle of sun-tracking solar aircraft is tightly related to the solar azimuth angle, which results in a large arc flight path to dynamically track the sun position. However, the limited detection range of payload usually requires solar aircraft to loiter over areas of interest for persistent surveillance missions. The large arc sun-tracking flight may cause the target area on the ground to be outside the maximum coverage area of payload. The present study therefore develops an optimal flight control approach for planning the flight path of sun-tracking solar aircraft within a mission region. The proposed method enables sun-tracking solar aircraft to maintain the optimal yawing angle most of the time during daylight flight, except when the aircraft reverses its direction by turning flight. For a circular region with a mission radius of 50 km, the optimal flight trajectory and controls of an example Λ-shaped sun-tracking solar aircraft are investigated theoretically. Results demonstrate the effectiveness of the proposed approach to optimize the flight path of the sun-tracking aircraft under the given circular region while maximizing the battery input power. Furthermore, the effects of varying the mission radius on energy performance are explored numerically. It has been proved that both net energy and energy balance remain nearly constant as the radius constraint varies, which enables the solar aircraft to achieve perpetual flight at almost the same latitude as the large arc flight. The method and results presented in this paper can provide reference for the persistent operation of sun-tracking solar aircraft within specific mission areas. 相似文献
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L. D. De Feiter 《Space Science Reviews》1974,16(1-2):3-43
In this paper a review is presented of the present status of our knowledge of solar flare phenomena with special emphasis on the production of suprathermal particles and their solar effects. Of these energetic particles electrons play an important role since they produce the X-ray and radiobursts observed during many flares. Also, during their slowing down to thermal energies they contribute to the heating of localized regions in the solar atmosphere, through energy exchange with the ambient electrons. Observable radiations of energetic protons, and other nuclei, are produced through nuclear interactions leading to the emissions of gamma-ray lines. Detectable fluxes of these gamma-ray lines are produced only in the most powerful flares. Also the nuclei that enter into deeper layers of the solar atmosphere transfer most of their kinetic energy to the ambient plasma. 相似文献
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P. B. Price 《Space Science Reviews》1973,15(1):69-88
The composition of cosmic rays and solar particles is reviewed with emphasis on the question of whether they are representative samples of Galactic and solar matter. The composition of solar particles changes with energy and from flare to flare. A strong excess of heavy elements at energies below a few MeV/nuc decreases with energy, and at energies above 15 MeV/nuc the composition of solar particles resembles that of galactic cosmic rays somewhat better than that of the solar atmosphere. The elements Ne through Pb have remarkably similar abundances in cosmic ray sources and in the matter of the solar system. The lighter elements are depleted in cosmic rays, whereas U and Th may be enriched or not, depending on whether the meteoritic or solar abundance of Th is used. Two prototype sources of cosmic rays are considered: gas with solar system composition but enriched in elements with Z > 8 during acceleration and emission (by analogy with solar particle emission), and highly evolved matter enriched in r-process elements such as U, Th and transuranic elements. The energy-dependence of cosmic ray composition suggests that both sources may contribute at different energies.Miller Institute Professor, 1972–73. 相似文献
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J.-A. Sauvaud D. Larson C. Aoustin D. Curtis J.-L. Médale A. Fedorov J. Rouzaud J. Luhmann T. Moreau P. Schröder P. Louarn I. Dandouras E. Penou 《Space Science Reviews》2008,136(1-4):227-239
SWEA, the solar wind electron analyzers that are part of the IMPACT in situ investigation for the STEREO mission, are described. They are identical on each of the two spacecraft. Both are designed to provide detailed measurements of interplanetary electron distribution functions in the energy range 1~3000 eV and in a 120°×360° solid angle sector. This energy range covers the core or thermal solar wind plasma electrons, and the suprathermal halo electrons including the field-aligned heat flux or strahl used to diagnose the interplanetary magnetic field topology. The potential of each analyzer will be varied in order to maintain their energy resolution for spacecraft potentials comparable to the solar wind thermal electron energies. Calibrations have been performed that show the performance of the devices are in good agreement with calculations and will allow precise diagnostics of all of the interplanetary electron populations at the two STEREO spacecraft locations. 相似文献
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Lyndsay Fletcher 《Space Science Reviews》2005,121(1-4):141-152
A solar flare is a violent and transient release of energy in the corona of the Sun, associated with the reconfiguration of
the coronal magnetic field. The major mystery of solar flare physics is the precise nature of the conversion of stored magnetic
energy into the copious accelerated particles that are observed indirectly by the radiation that they produce, and also directly
with in situ detectors. This presents a major challenge for theory and modeling. Recent years have brought significant observational
advances in the study of solar flares, addressing the storage and release of magnetic energy, and the acceleration and propagation
of fast electrons and ions. This paper concentrates on two topics relevant to the early phase of a flare, magnetic reconnection
and charged particle acceleration and transport. Some recent pertinent observations are reviewed and pointers given for the
directions that, this reviewer suggests, computational models should now seek to take. 相似文献
18.
Converting the solar energy received on the surface of the Earth has not been practical with heat engines because of the low density of this energy. On a clear bright day in the summer, the sun generally delivers less than 80 W per square foot. Also, heat engines are prohibited from exceeding the Carnot-cycle efficiency limit. On the other hand, plants perform their energy conversion electrochemically, and, hence, are not limited by the Carnot-cycle. They use solar energy to produce useful fuels that range from corn-cobs and maple syrup to pitch and firewood. However, they have an extremely complicated process control that uses blue and red parts of the visible solar spectrum to extract hydrogen from water and carbon from carbon dioxide to make hydrocarbons. They do not need precious-metal catalysts; however they run complex data processing programs in which stored instructions control electrochemical reactions and also cause growth and production of needed products to occur when needed. 相似文献
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太阳能/氢能无人机总体设计与能源管理策略研究 总被引:2,自引:2,他引:2
针对小型低空长航时电动无人机需求,给出了太阳能/氢能混合能源动力系统集成方案和小型低空长航时无人机构型。针对典型任务剖面,综合考虑太阳能电池和氢燃料电池特性,提出了一种考虑全机重量能量耦合关系的总体设计方法和任务剖面驱动的能源管理策略;建立了能源系统模型,给出了能源控制流程,开发了能源管理仿真平台。以1.5 kg任务载荷为例,完成了无人机总体方案设计,仿真分析了各种能源特性对飞行结果的影响。结果表明:能源管理策略能够根据任务剖面的要求合理配置能源系统的功率,满足各阶段的功率需求;无人机在冬至日航时为21 h、夏至日可实现跨昼夜飞行;在能源系统重量相同情况下,该混合能源无人机的航时分别是纯锂电池无人机和燃料电池无人机的5.5倍和1.2倍。 相似文献
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Eckart Marsch 《Space Science Reviews》2012,172(1-4):23-39
The radial evolution of the velocity distribution functions of the protons, electrons and ions, as they were measured during the Helios mission in the solar wind between 0.3 and 1.0 AU, is discussed and analysed. Emphasis is placed on the detailed plasma measurements, and on the non-thermal features of the particles and the kinetic processes they undergo in the expanding solar wind. As the plasma is multi-component and nonuniform, complexity prevails and the observed distributions exhibit, owing to their low number densities, significant deviations from local thermal equilibrium, and reveal such suprathermal particles as the strahl electrons, as well as ion beams and temperature anisotropies. The distribution functions still carry imprints of their solar boundaries that are reflected locally, but also have ample free energy driving in situ plasma instabilities which are triggered and modulated by wave-particle interactions. The ion temperatures and their anisotropies and the non-adiabatic radial evolution of the solar wind internal energy are discussed in detail. 相似文献