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981.
H. Nilsson R. Lundin K. Lundin S. Barabash H. Borg O. Norberg A. Fedorov J.-A Sauvaud H. Koskinen E. Kallio P. Riihelä J. L. Burch 《Space Science Reviews》2007,128(1-4):671-695
The Ion Composition Analyzer (ICA) is part of the Rosetta Plasma Consortium (RPC). ICA is designed to measure the three-dimensional
distribution function of positive ions in order to study the interaction between the solar wind and cometary particles. The
instrument has a mass resolution high enough to resolve the major species such as protons, helium, oxygen, molecular ions,
and heavy ions characteristic of dusty plasma regions. ICA consists of an electrostatic acceptance angle filter, an electrostatic
energy filter, and a magnetic momentum filter. Particles are detected using large diameter (100 mm) microchannel plates and
a two-dimensional anode system. ICA has its own processor for data reduction/compression and formatting. The energy range
of the instrument is from 25 eV to 40 keV and an angular field-of-view of 360° × 90° is achieved through electrostatic deflection
of incoming particles. 相似文献
982.
The Geology of Mercury: The View Prior to the MESSENGER Mission 总被引:1,自引:0,他引:1
James W. Head Clark R. Chapman Deborah L. Domingue S. Edward Hawkins III William E. McClintock Scott L. Murchie Louise M. Prockter Mark S. Robinson Robert G. Strom Thomas R. Watters 《Space Science Reviews》2007,131(1-4):41-84
Mariner 10 and Earth-based observations have revealed Mercury, the innermost of the terrestrial planetary bodies, to be an
exciting laboratory for the study of Solar System geological processes. Mercury is characterized by a lunar-like surface,
a global magnetic field, and an interior dominated by an iron core having a radius at least three-quarters of the radius of
the planet. The 45% of the surface imaged by Mariner 10 reveals some distinctive differences from the Moon, however, with
major contractional fault scarps and huge expanses of moderate-albedo Cayley-like smooth plains of uncertain origin. Our current
image coverage of Mercury is comparable to that of telescopic photographs of the Earth’s Moon prior to the launch of Sputnik
in 1957. We have no photographic images of one-half of the surface, the resolution of the images we do have is generally poor
(∼1 km), and as with many lunar telescopic photographs, much of the available surface of Mercury is distorted by foreshortening
due to viewing geometry, or poorly suited for geological analysis and impact-crater counting for age determinations because
of high-Sun illumination conditions. Currently available topographic information is also very limited. Nonetheless, Mercury
is a geological laboratory that represents (1) a planet where the presence of a huge iron core may be due to impact stripping
of the crust and upper mantle, or alternatively, where formation of a huge core may have resulted in a residual mantle and
crust of potentially unusual composition and structure; (2) a planet with an internal chemical and mechanical structure that
provides new insights into planetary thermal history and the relative roles of conduction and convection in planetary heat
loss; (3) a one-tectonic-plate planet where constraints on major interior processes can be deduced from the geology of the
global tectonic system; (4) a planet where volcanic resurfacing may not have played a significant role in planetary history
and internally generated volcanic resurfacing may have ceased at ∼3.8 Ga; (5) a planet where impact craters can be used to
disentangle the fundamental roles of gravity and mean impactor velocity in determining impact crater morphology and morphometry;
(6) an environment where global impact crater counts can test fundamental concepts of the distribution of impactor populations
in space and time; (7) an extreme environment in which highly radar-reflective polar deposits, much more extensive than those
on the Moon, can be better understood; (8) an extreme environment in which the basic processes of space weathering can be
further deduced; and (9) a potential end-member in terrestrial planetary body geological evolution in which the relationships
of internal and surface evolution can be clearly assessed from both a tectonic and volcanic point of view. In the half-century
since the launch of Sputnik, more than 30 spacecraft have been sent to the Moon, yet only now is a second spacecraft en route
to Mercury. The MESSENGER mission will address key questions about the geologic evolution of Mercury; the depth and breadth
of the MESSENGER data will permit the confident reconstruction of the geological history and thermal evolution of Mercury
using new imaging, topography, chemistry, mineralogy, gravity, magnetic, and environmental data. 相似文献
983.
ARTEMIS Science Objectives 总被引:1,自引:0,他引:1
D. G. Sibeck V. Angelopoulos D. A. Brain G. T. Delory J. P. Eastwood W. M. Farrell R. E. Grimm J. S. Halekas H. Hasegawa P. Hellinger K. K. Khurana R. J. Lillis M. ?ieroset T.-D. Phan J. Raeder C. T. Russell D. Schriver J. A. Slavin P. M. Travnicek J. M. Weygand 《Space Science Reviews》2011,165(1-4):59-91
NASA??s two spacecraft ARTEMIS mission will address both heliospheric and planetary research questions, first while in orbit about the Earth with the Moon and subsequently while in orbit about the Moon. Heliospheric topics include the structure of the Earth??s magnetotail; reconnection, particle acceleration, and turbulence in the Earth??s magnetosphere, at the bow shock, and in the solar wind; and the formation and structure of the lunar wake. Planetary topics include the lunar exosphere and its relationship to the composition of the lunar surface, the effects of electric fields on dust in the exosphere, internal structure of the Moon, and the lunar crustal magnetic field. This paper describes the expected contributions of ARTEMIS to these baseline scientific objectives. 相似文献
984.
The Heavy Ion Counter on the Galileo spacecraft will monitor energetic heavy nuclei of the elements from C to Ni, with energies from 6 to 200 MeV nucl-1. The instrument will provide measurements of trapped heavy ions in the Jovian magnetosphere, including those high-energy heavy ions with the potential for affecting the operation of the spacecraft electronic circuitry. We describe the instrument, which is a modified version of the Voyager CRS instrument. 相似文献
985.
跨声速翼型绕流的Euler/边界层方程干扰数值解 总被引:2,自引:0,他引:2
本文利用Euler方程和可压缩湍流边界层积分方程研究绕跨声速翼型的有粘与无粘强干扰流动。应用有限差分法在贴体的网格上求解时间相关的Euler方程,以剪功积分方法求解翼面贴附和分离湍流边界层流动,并引入一个松弛方程描述剪应力对上游湍流历程的延迟响应。有粘/无粘干扰采用表面源模型。计算结果表明,对翼面存在强干扰流动情况,获得了与实验值基本吻合的结果。 相似文献
986.
987.
介绍一种二元进气道模型在非均匀超音来流中的初步研究结果。试验在DLR小型超音风洞上进行。为造成非均匀来流条件,试验中将部分或全部试验段顶壁附面层引入进气道模型。结果表明,进气斜板产生的头激波与来流附面层相互作用的性状在不同的附面层隔道下变化极大。随隔道高度增加,激波附面层相互作用距离L起初亦增加,当全部附面层被排移后,L大幅度下降。与均匀来流试验结果相比较,当来流顶壁附面层全部被进气道吞入时,该进气道总压恢复σ及质量流率m分别降低18%及15%(M_∞=2.19),同时出口面总压畸变大幅度增加。文章分析了原因及对进气道性能影响的强度。 相似文献
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