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991.
Lembege B. Giacalone J. Scholer M. Hada T. Hoshino M. Krasnoselskikh V. Kucharek H. Savoini P. Terasawa T. 《Space Science Reviews》2004,110(3-4):161-226
The physics of collisionless shocks is a very broad topic, which has been well studied for many decades. However, there are a number of important issues which remain unresolved. Moreover, there have been new findings, which cast doubt on well-established ideas. The purpose of this review is to address a subset of unresolved problems in collisionless shock physics from a theoretical and/or numerical modeling point of view. The topics which are addressed are: the nonstationarity of the shock front, the heating and dynamics of electrons through the shock layer, particle diffusion in turbulent electric and magnetic fields, particle acceleration, and the interaction of pickup ions with collisionless shocks. 相似文献
992.
Øieroset Marit Mitchell David L. Phan Tai D. Lin Robert P. Crider Dana H. Acuña Mario H. 《Space Science Reviews》2004,111(1-2):185-202
Using magnetometer and electron observations from the Mars Global Surveyor (MGS) and the Wind spacecraft we show that the region of magnetic field pile-up and density decrease located between the Martian ionosphere and bow shock exhibit strong similarities with the plasma depletion layer (PDL) observed upstream of the Earth's magnetopause in the absence of magnetic reconnection when the magnetopause is a solid obstacle in the solar wind. A PDL is formed upstream of the terrestrial magnetopause when the magnetic field piles up against the obstacle and particles in the pile-up region are squeezed away from the high magnetic pressure region along the field lines as the flux tubes convect toward the magnetopause. We here discuss the possibility that at least part of the region of magnetic field pile-up and density depletion upstream of Mars may be formed by the same physical processes which generate the PDL upstream of the Earth's magnetopause. More complete ion, electron, and neutral measurements are needed to conclusively determine the relative importance of the plasma depletion process versus exospheric processes. 相似文献
993.
P. C. Frisch M. Bzowski E. Grün V. Izmodenov H. Krüger J. L. Linsky D. J. McComas E. Möbius S. Redfield N. Schwadron R. Shelton J. D. Slavin B. E. Wood 《Space Science Reviews》2009,146(1-4):235-273
Interstellar material (ISMa) is observed both inside and outside of the heliosphere. Relating these diverse sets of ISMa data provides a richer understanding of both the interstellar medium and the heliosphere. The galactic environment of the Sun is dominated by warm, low-density, partially ionized interstellar material consisting of atoms and dust grains. The properties of the heliosphere are dependent on the pressure, composition, radiation field, ionization, and magnetic field of ambient ISMa. The very low-density interior of the Local Bubble, combined with an expanding superbubble shell associated with star formation in the Scorpius-Centaurus Association, dominate the properties of the local interstellar medium (LISM). Once the heliosphere boundaries and interaction mechanisms are understood, interstellar gas, dust, pickup ions, and anomalous cosmic rays inside of the heliosphere can be directly compared to ISMa outside of the heliosphere. Our understanding of ISMa at the Sun is further enriched when the circumheliospheric interstellar material is compared to observations of other nearby ISMa and the overall context of our galactic environment. The IBEX mission will map the interaction region between the heliosphere and ISMa, and improve the accuracy of comparisons between ISMa inside and outside the heliosphere. 相似文献
994.
D. McComas F. Allegrini F. Bagenal P. Casey P. Delamere D. Demkee G. Dunn H. Elliott J. Hanley K. Johnson J. Langle G. Miller S. Pope M. Reno B. Rodriguez N. Schwadron P. Valek S. Weidner 《Space Science Reviews》2008,140(1-4):261-313
The Solar Wind Around Pluto (SWAP) instrument on New Horizons will measure the interaction between the solar wind and ions created by atmospheric loss from Pluto. These measurements provide a characterization of the total loss rate and allow us to examine the complex plasma interactions at Pluto for the first time. Constrained to fit within minimal resources, SWAP is optimized to make plasma-ion measurements at all rotation angles as the New Horizons spacecraft scans to image Pluto and Charon during the flyby. To meet these unique requirements, we combined a cylindrically symmetric retarding potential analyzer with small deflectors, a top-hat analyzer, and a redundant/coincidence detection scheme. This configuration allows for highly sensitive measurements and a controllable energy passband at all scan angles of the spacecraft. 相似文献
995.
The THEMIS Fluxgate Magnetometer 总被引:2,自引:0,他引:2
H. U. Auster K. H. Glassmeier W. Magnes O. Aydogar W. Baumjohann D. Constantinescu D. Fischer K. H. Fornacon E. Georgescu P. Harvey O. Hillenmaier R. Kroth M. Ludlam Y. Narita R. Nakamura K. Okrafka F. Plaschke I. Richter H. Schwarzl B. Stoll A. Valavanoglou M. Wiedemann 《Space Science Reviews》2008,141(1-4):235-264
996.
Infrared signature studies of aerospace vehicles 总被引:8,自引:0,他引:8
Shripad P. Mahulikar Hemant R. Sonawane G. Arvind Rao 《Progress in Aerospace Sciences》2007,43(7-8):218-245
Infrared (IR) emissions from aircraft are used to detect, track, and lock-on to the target. MAN Portable Air Defence Systems (MANPADS) have emerged as a major cause of aircraft and helicopter loss. Therefore, IR signature studies are important to counter this threat for survivability enhancement, and are an important aspect of stealth technology. This paper reviews contemporary developments in this discipline, with particular emphasis on IR signature prediction from aerospace vehicles. The role of atmosphere in IR signature analysis, and relation between IR signature level and target susceptibility are illustrated. Also, IR signature suppression systems and countermeasure techniques are discussed, to highlight their effectiveness and implications in terms of penalties. 相似文献
997.
S. A. Stern D. C. Slater J. Scherrer J. Stone M. Versteeg M. F. A’hearn J. L. Bertaux P. D. Feldman M. C. Festou Joel Wm. Parker O. H. W. Siegmund 《Space Science Reviews》2007,128(1-4):507-527
We describe the design, performance and scientific objectives of the NASA-funded ALICE instrument aboard the ESA Rosetta asteroid flyby/comet rendezvous mission. ALICE is a lightweight, low-power, and low-cost imaging spectrograph optimized for cometary far-ultraviolet (FUV) spectroscopy. It will be the first UV spectrograph to study a comet at close range. It is designed to obtain spatially-resolved spectra of Rosetta mission targets in the 700–2050 Å spectral band with a spectral resolution between 8 Å and 12 Å for extended sources that fill its ~0.05^ × 6.0^ field-of-view. ALICE employs an off-axis telescope feeding a 0.15-m normal incidence Rowland circle spectrograph with a toroidal concave holographic reflection grating. The microchannel plate detector utilizes dual solar-blind opaque photocathodes (KBr and CsI) and employs a two-dimensional delay-line readout array. The instrument is controlled by an internal microprocessor. During the prime Rosetta mission, ALICE will characterize comet 67P/Churyumov-Gerasimenko's coma, its nucleus, and nucleus/coma coupling; during cruise to the comet, ALICE will make observations of the mission's two asteroid flyby targets and of Mars, its moons, and of Earth's moon. ALICE has already successfully completed the in-flight commissioning phase and is operating well in flight. It has been characterized in flight with stellar flux calibrations, observations of the Moon during the first Earth fly-by, and observations of comet C/2002 T7 (LINEAR) in 2004 and comet 9P/Tempel 1 during the 2005 Deep Impact comet-collision observing campaign. 相似文献
998.
C. Giammanco P. Bochsler R. Karrer F. M. Ipavich J. A. Paquette P. Wurz 《Space Science Reviews》2007,130(1-4):329-333
Solar chemical abundances are determined by comparing solar photospheric spectra with synthetic ones obtained for different
sets of abundances and physical conditions. Although such inferred results are reliable, they are model dependent. Therefore,
one compares them with the values for the local interstellar medium (LISM). The argument is that they must be similar, but
even for LISM abundance determinations models play a fundamental role (i.e., temperature fluctuations, clumpiness, photon
leaks). There are still two possible comparisons—one with the meteoritic values and the second with solar wind abundances.
In this work we derive a first estimation of the solar wind element ratios of sulfur relative to calcium and magnesium, two
neighboring low-FIP elements, using 10 years of CELIAS/MTOF data. We compare the sulfur abundance with the abundance determined
from spectroscopic observations and from solar energetic particles. Sulfur is a moderately volatile element, hence, meteoritic
sulfur may be depleted relative to non-volatile elements, if compared to its original solar system value. 相似文献
999.
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
1000.
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