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排序方式: 共有123条查询结果,搜索用时 31 毫秒
71.
Larry W. Esposito Charles A. Barth Joshua E. Colwell George M. Lawrence William E. McClintock A. Ian F. Stewart H. Uwe Keller Axel Korth Hans Lauche Michel C. Festou Arthur L. Lane Candice J. Hansen Justin N. Maki Robert A. West Herbert Jahn Ralf Reulke Kerstin Warlich Donald E. Shemansky Yuk L. Yung 《Space Science Reviews》2004,115(1-4):299-361
The Cassini Ultraviolet Imaging Spectrograph (UVIS) is part of the remote sensing payload of the Cassini orbiter spacecraft. UVIS has two spectrographic channels that provide images and spectra covering the ranges from 56 to 118 nm and 110 to 190 nm. A third optical path with a solar blind CsI photocathode is used for high signal-to-noise-ratio stellar occultations by rings and atmospheres. A separate Hydrogen Deuterium Absorption Cell measures the relative abundance of deuterium and hydrogen from their Lyman-α emission. The UVIS science objectives include investigation of the chemistry, aerosols, clouds, and energy balance of the Titan and Saturn atmospheres; neutrals in the Saturn magnetosphere; the deuterium-to-hydrogen (D/H) ratio for Titan and Saturn; icy satellite surface properties; and the structure and evolution of Saturn’s rings.This revised version was published online in July 2005 with a corrected cover date. 相似文献
72.
In vivo and in vitro measurements of complex-type chromosomal exchanges induced by heavy ions. 总被引:3,自引:0,他引:3
K George M Durante H Wu V Willingham F A Cucinotta 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2003,31(6):1525-1535
Heavy ions are more efficient in producing complex-type chromosome exchanges than sparsely ionizing radiation, and this can potentially be used as a biomarker of radiation quality. We measured the induction of complex-type chromosomal aberrations in human peripheral blood lymphocytes exposed in vitro to accelerated H-, He-, C-, Ar-, Fe- and Au-ions in the LET range of approximately 0.4-1400 keV/micrometers. Chromosomes were analyzed either at the first post-irradiation mitosis, or in interphase, following premature condensation by phosphatase inhibitors. Selected chromosomes were then visualized after FISH-painting. The dose-response curve for the induction of complex-type exchanges by heavy ions was linear in the dose-range 0.2-1.5 Gy, while gamma-rays did not produce a significant increase in the yield of complex rearrangements in this dose range. The yield of complex aberrations after 1 Gy of heavy ions increased up to an LET around 100 keV/micrometers, and then declined at higher LET values. When mitotic cells were analyzed, the frequency of complex rearrangements after 1 Gy was about 10 times higher for Ar- or Fe- ions (the most effective ions, with LET around 100 keV/micrometers) than for 250 MeV protons, and values were about 35 times higher in prematurely condensed chromosomes. These results suggest that complex rearrangements may be detected in astronauts' blood lymphocytes after long-term space flight, because crews are exposed to HZE particles from galactic cosmic radiation. However, in a cytogenetic study of ten astronauts after long-term missions on the Mir or International Space Station, we found a very low frequency of complex rearrangements, and a significant post-flight increase was detected in only one out of the ten crewmembers. It appears that the use of complex-type exchanges as biomarker of radiation quality in vivo after low-dose chronic exposure in mixed radiation fields is hampered by statistical uncertainties. 相似文献
73.
The Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) on the New Horizons Mission
Ralph L. McNutt Jr. Stefano A. Livi Reid S. Gurnee Matthew E. Hill Kim A. Cooper G. Bruce Andrews Edwin P. Keath Stamatios M. Krimigis Donald G. Mitchell Barry Tossman Fran Bagenal John D. Boldt Walter Bradley William S. Devereux George C. Ho Stephen E. Jaskulek Thomas W. LeFevere Horace Malcom Geoffrey A. Marcus John R. Hayes G. Ty Moore Mark E. Perry Bruce D. Williams Paul Wilson IV Lawrence E. Brown Martha B. Kusterer Jon D. Vandegriff 《Space Science Reviews》2008,140(1-4):315-385
The Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) comprises the hardware and accompanying science investigation on the New Horizons spacecraft to measure pick-up ions from Pluto’s outgassing atmosphere. To the extent that Pluto retains its characteristics similar to those of a “heavy comet” as detected in stellar occultations since the early 1980s, these measurements will characterize the neutral atmosphere of Pluto while providing a consistency check on the atmospheric escape rate at the encounter epoch with that deduced from the atmospheric structure at lower altitudes by the ALICE, REX, and SWAP experiments on New Horizons. In addition, PEPSSI will characterize any extended ionosphere and solar wind interaction while also characterizing the energetic particle environment of Pluto, Charon, and their associated system. First proposed for development for the Pluto Express mission in September 1993, what became the PEPSSI instrument went through a number of development stages to meet the requirements of such an instrument for a mission to Pluto while minimizing the required spacecraft resources. The PEPSSI instrument provides for measurements of ions (with compositional information) and electrons from 10 s of keV to ~1 MeV in a 160°×12° fan-shaped beam in six sectors for 1.5 kg and ~2.5 W. 相似文献
74.
James C. Leary Richard F. Conde George Dakermanji Carl S. Engelbrecht Carl J. Ercol Karl B. Fielhauer David G. Grant Theodore J. Hartka Tracy A. Hill Stephen E. Jaskulek Mary A. Mirantes Larry E. Mosher Michael V. Paul David F. Persons Elliot H. Rodberg Dipak K. Srinivasan Robin M. Vaughan Samuel R. Wiley 《Space Science Reviews》2007,131(1-4):187-217
The MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft was designed and constructed to withstand the harsh environments associated with achieving and operating in Mercury
orbit. The system can be divided into eight subsystems: structures and mechanisms (e.g., the composite core structure, aluminum
launch vehicle adapter, and deployables), propulsion (e.g., the state-of-the-art titanium fuel tanks, thruster modules, and
associated plumbing), thermal (e.g., the ceramic-cloth sunshade, heaters, and radiators), power (e.g., solar arrays, battery,
and controlling electronics), avionics (e.g., the processors, solid-state recorder, and data handling electronics), software
(e.g., processor-supported code that performs commanding, data handling, and spacecraft control), guidance and control (e.g.,
attitude sensors including star cameras and Sun sensors integrated with controllers including reaction wheels), radio frequency
telecommunications (e.g., the spacecraft antenna suites and supporting electronics), and payload (e.g., the science instruments
and supporting processors). This system architecture went through an extensive (nearly four-year) development and testing
effort that provided the team with confidence that all mission goals will be achieved.
Larry E. Mosher passed away during the preparation of this paper. 相似文献
75.
K George V Willingham H Wu D Gridley G Nelson F A Cucinotta 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2002,30(4):891-899
Although the space radiation environment consists predominantly of energetic protons, astronauts inside a spacecraft are chronically exposed to both primary particles as well as secondary particles that are generated when the primary particles penetrate the spacecraft shielding. Secondary neutrons and secondary charged particles can have an LET value that is greater than the primary protons and, therefore, produce a higher relative biological effectiveness (RBE). Using the accelerator facility at Loma Linda University, we exposed human lymphocytes in vitro to 250 MeV protons with doses ranging from 0 to 60 cGy at three different dose rates: a low dose rate of 7.5 cGy/h, an intermediate dose rate of 30 cGy/h and a high dose rate of 70 cGy/min. The effect of 15 g/cm2 aluminum shielding on the induction of chromosome aberrations was investigated for each dose rate. After exposure, lymphocytes were incubated in growth medium containing phytohemagglutinin (PHA) and chromosome spreads were collected using a chemical-induced premature chromosome condensation (PCC) technique. Aberrations were analyzed using the fluorescence in situ hybridization (FISH) technique with three different colored chromosome-painting probes. The frequency of reciprocal and complex-type chromosome exchanges were compared in shielded and unshielded samples. 相似文献
76.
Planetary upper atmospheres-coexisting thermospheres and ionospheres-form an important boundary between the planet itself
and interplanetary space. The solar wind and radiation from the Sun may react with the upper atmosphere directly, as in the
case of Venus. If the planet has a magnetic field, however, such interactions are mediated by the magnetosphere, as in the
case of the Earth. All of the Solar System’s giant planets have magnetic fields of various strengths, and interactions with
their space environments are thus mediated by their respective magnetospheres. This article concentrates on the consequences
of magnetosphere-atmosphere interactions for the physical conditions of the thermosphere and ionosphere. In particular, we
wish to highlight important new considerations concerning the energy balance in the upper atmosphere of Jupiter and Saturn,
and the role that coupling between the ionosphere and thermosphere may play in establishing and regulating energy flows and
temperatures there. This article also compares the auroral activity of Earth, Jupiter, Saturn and Uranus. The Earth’s behaviour
is controlled, externally, by the solar wind. But Jupiter’s is determined by the co-rotation or otherwise of the equatorial
plasmasheet, which is internal to the planet’s magnetosphere. Despite being rapid rotators, like Jupiter, Saturn and Uranus
appear to have auroral emissions that are mainly under solar (wind) control. For Jupiter and Saturn, it is shown that Joule
heating and “frictional” effects, due to ion-neutral coupling can produce large amounts of energy that may account for their
high exospheric temperatures. 相似文献
77.
The James Webb Space Telescope 总被引:4,自引:0,他引:4
Jonathan P. Gardner John C. Mather Mark Clampin Rene Doyon Matthew A. Greenhouse Heidi B. Hammel John B. Hutchings Peter Jakobsen Simon J. Lilly Knox S. Long Jonathan I. Lunine Mark J. Mccaughrean Matt Mountain John Nella George H. Rieke Marcia J. Rieke Hans-Walter Rix Eric P. Smith George Sonneborn Massimo Stiavelli H. S. Stockman Rogier A. Windhorst Gillian S. Wright 《Space Science Reviews》2006,123(4):485-606
The James Webb Space Telescope (JWST) is a large (6.6 m), cold (<50 K), infrared (IR)-optimized space observatory that will be launched early in the next decade into orbit around the second Earth–Sun Lagrange point. The observatory will have four instruments: a near-IR camera, a near-IR multiobject spectrograph, and a tunable filter imager will cover the wavelength range, 0.6 < ; < 5.0 μ m, while the mid-IR instrument will do both imaging and spectroscopy from 5.0 < ; < 29 μ m.The JWST science goals are divided into four themes. The key objective of The End of the Dark Ages: First Light and Reionization theme is to identify the first luminous sources to form and to determine the ionization history of the early universe. The key objective of The Assembly of Galaxies theme is to determine how galaxies and the dark matter, gas, stars, metals, morphological structures, and active nuclei within them evolved from the epoch of reionization to the present day. The key objective of The Birth of Stars and Protoplanetary Systems theme is to unravel the birth and early evolution of stars, from infall on to dust-enshrouded protostars to the genesis of planetary systems. The key objective of the Planetary Systems and the Origins of Life theme is to determine the physical and chemical properties of planetary systems including our own, and investigate the potential for the origins of life in those systems. Within these themes and objectives, we have derived representative astronomical observations.To enable these observations, JWST consists of a telescope, an instrument package, a spacecraft, and a sunshield. The telescope consists of 18 beryllium segments, some of which are deployed. The segments will be brought into optical alignment on-orbit through a process of periodic wavefront sensing and control. The instrument package contains the four science instruments and a fine guidance sensor. The spacecraft provides pointing, orbit maintenance, and communications. The sunshield provides passive thermal control. The JWST operations plan is based on that used for previous space observatories, and the majority of JWST observing time will be allocated to the international astronomical community through annual peer-reviewed proposal opportunities. 相似文献
78.
Zoe Szajnfarber Thomas M.K. Coles George R. Sondecker Anthony C. Wicht Annalisa L. Weigel 《Space Policy》2011,27(3):131-145
This paper analyses potential future collaborative space exploration architectures in terms of 1) the technical capabilities of contributing partners; and 2) the constraints imposed by internal and international politics. We find that when international partners are considered endogenously, the argument for a “flexible path” approach is weakened substantially. This is because international contributions can make “Moon first” economically feasible; and characteristics of proposed “flexible path” approaches may preclude international involvement because of the disproportionate risk that those contributions inherently bear. This could have serious implications for future collaborations. We also note that while there are multiple feasible collaborative architectures, there is currently substantial overlap among the potential niche contributions identified by the international partners. 相似文献
79.
Observations and measurements in the solar wind, the Jovian atmosphere and the gases trapped in lunar surface material provide
the main evidence from which the isotopic composition of H, He and Ne in the Protosolar Cloud (PSC) is derived. These measurements
and observations are reviewed and the corrections are discussed that are needed for obtaining from them the PSC isotopic ratios.
The D/H, 3He/4He (D+3He)/H, 20Ne/22Ne and 21Ne/22Ne ratios adopted for the PSC are presented. Protosolar abundances provide the basis for the interpretation of isotopic ratios
measured in the various solar system objects. In this article we discuss constraints derived from the PSC abundances on solar
mixing, the origin of atmospheric neon, and the nature of the “SEP” component of neon trapped at the lunar surface. We also
discuss constraints on the galactic evolution provided by the isotopic abundances of H and He in the PSC.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
80.
Chalfin Albert Staton George R. 《IEEE transactions on aerospace and electronic systems》1966,(3):291-302
A tactical system designed to inspect and diagnose malfunctions in all army tactical vehicles including jeeps, trucks, and tanks is known as Ready Multipurpose Automatic Inspection and Diagnostic System (READYMAIDS). The laboratory model developed to prove the feasibility of design is discussed together with design problems such as instrumenting a vehicle without modifications. The system uses a small digital computer in addition to switching, measurement, and loading devices. These devices are integrated into a small transportable unit. Results to date, problem areas, and possible solutions are described. 相似文献