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51.
Metallic ions coming from the ablation of extraterrestrial dust, play a significant role in the distribution of ions in the Earth’s ionosphere. Ions of magnesium and iron, and to a lesser extent, sodium, aluminium, calcium and nickel, are a permanent feature of the lower E-region. The presence of interplanetary dust at long distances from the Sun has been confirmed by the measurements obtained by several spacecrafts. As on Earth, the flux of interplanetary meteoroids can affect the ionospheric structure of other planets. The electron density of many planets show multiple narrow layers below the main ionospheric peak which are similar, in magnitude, to the upper ones. These layers could be due to long-lived metallic ions supplied by interplanetary dust and/or their satellites. In the case of Mars, the presence of a non-permanent ionospheric layer at altitudes ranging from 65 to 110 km has been confirmed and the ion Mg+?CO2 identified. Here we present a review of the present status of observed low ionospheric layers in Venus, Mars, Jupiter, Saturn and Neptune together with meteoroid based models to explain the observations. Meteoroids could also affect the ionospheric structure of Titan, the largest Saturnian moon, and produce an ionospheric layer at around 700 km that could be investigated by Cassini. 相似文献
52.
In the first half of the 20th century, Leonard Ornstein turned the Physics Laboratory of Utrecht University into a center for testing the nascent quantum mechanics through accurate measurements of line intensities in flame spectra. The microphotometer of instrument builder Willem Moll was the key to this success. Marcel Minneart used this instrument to study stellar spectra at the Utrecht Astronomical Institute, and in particular for the Photometric Atlas of the Solar Spectrum. When the opportunity came in the 1960s to build instruments for research from space, it was natural that Kees de Jager opted for spectroscopy, in X-ray observations of the Sun. The expertise developed in this program allowed the Space Research Organisation of the Netherlands to be a principal player in the development of X-ray spectrographs on the Einstein, EXOSAT, Chandra and XMM-Newton satellites. 相似文献
53.
Aubrey AD Chalmers JH Bada JL Grunthaner FJ Amashukeli X Willis P Skelley AM Mathies RA Quinn RC Zent AP Ehrenfreund P Amundson R Glavin DP Botta O Barron L Blaney DL Clark BC Coleman M Hofmann BA Josset JL Rettberg P Ride S Robert F Sephton MA Yen A 《Astrobiology》2008,8(3):583-595
The Urey organic and oxidant detector consists of a suite of instruments designed to search for several classes of organic molecules in the martian regolith and ascertain whether these compounds were produced by biotic or abiotic processes using chirality measurements. These experiments will also determine the chemical stability of organic molecules within the host regolith based on the presence and chemical reactivity of surface and atmospheric oxidants. Urey has been selected for the Pasteur payload on the European Space Agency's (ESA's) upcoming 2013 ExoMars rover mission. The diverse and effective capabilities of Urey make it an integral part of the payload and will help to achieve a large portion of the mission's primary scientific objective: "to search for signs of past and present life on Mars." This instrument is named in honor of Harold Urey for his seminal contributions to the fields of cosmochemistry and the origin of life. 相似文献
54.
Frank Sohl Mathieu Choukroun Jeffrey Kargel Jun Kimura Robert Pappalardo Steve Vance Mikhail Zolotov 《Space Science Reviews》2010,153(1-4):485-510
The state of knowledge about the structure and composition of icy satellite interiors has been significantly extended by combining direct measurements from spacecraft, laboratory experiments, and theoretical modeling. The existence of potentially habitable liquid water reservoirs on icy satellites is dependent on the radiogenic heating of the rock component, additional contributions such as the dissipation of tidal energy, the efficiency of heat transfer to the surface, and the presence of substances that deplete the freezing point of liquid water. This review summarizes the chemical evolution of subsurface liquid water oceans, taking into account a number of chemical processes occuring in aqueous environments and partly related to material exchange with the deep interior. Of interest are processes occuring at the transitions from the liquid water layer to the ice layers above and below, involving the possible formation of clathrate hydrates and high-pressure ices on large icy satellites. In contrast, water-rock exchange is important for the chemical evolution of the liquid water layer if the latter is in contact with ocean floor rock on small satellites. The composition of oceanic floor deposits depends on ambient physical conditions and ocean chemistry, and their evolutions through time. In turn, physical properties of the ocean floor affect the circulation of oceanic water and related thermal effects due to tidally-induced porous flow and aqueous alteration of ocean floor rock. 相似文献
55.
Effects of ice accretions on aircraft aerodynamics 总被引:13,自引:0,他引:13
This article is a systematic and comprehensive review, correlation, and assessment of test results available in the public domain which address the aerodynamic performance and control degradations caused by various types of ice accretions on the lifting surfaces of fixed wing aircraft. To help put the various test results in perspective, overviews are provided first of the important factors and limitations involved in computational and experimental icing simulation techniques, as well as key aerodynamic testing simulation variables and governing flow physics issues. Following these are the actual reviews, assessments, and correlations of a large number of experimental measurements of various forms of mostly simulated in-flight and ground ice accretions, augmented where appropriate by similar measurements for other analogous forms of surface contamination and/or disruptions. In-flight icing categories reviewed include the initial and inter-cycle ice accretions inherent in the use of de-icing systems which are of particular concern because of widespread misconceptions about the thickness of such accretions which can be allowed before any serious consequences occur, and the runback/ridge ice accretions typically associated with larger-than-normal water droplet encounters which are of major concern because of the possible potential for catastrophic reductions in aerodynamic effectiveness. The other in-flight ice accretion category considered includes the more familiar large rime and glaze ice accretions, including ice shapes with rather grotesque features, where the concern is that, in spite of all the research conducted to date, the upper limit of penalties possible has probably not been defined. Lastly, the effects of various possible ground frost/ice accretions are considered. The concern with some of these is that for some types of configurations, all of the normally available operating margins to stall at takeoff may be erased if these accretions are not adequately removed prior to takeoff. Throughout this review, important voids in the available database are highlighted, as are instances where previous lessons learned have tended to be overlooked. 相似文献
56.
Willem W. Verstraeten Frank Veroustraete Walter Heyns Tom Van Roey Jan Feyen 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2008,41(1):20-35
Uncertainty on carbon fluxes is determined by the uncertainties of ecosystem model structure, data and model parameter uncertainties and the temporal and spatial inaccuracy of the input data retrieval. The objective of this paper is to understand the error propagation and uncertainty of evaporative fraction (EF), soil moisture content (SMC) and water limited net ecosystem productivity (NEP). In this respect, C-Fix and spaceborne remote sensing are used for the ‘Brasschaat’ pixel. A simple model based on error theory and a Monte-Carlo approach are used. Different error scenarios are implemented to assess input uncertainty on EF, SMC and NEP as estimated with C-Fix. 相似文献
57.
Hsien Shang Frank H. Shu Typhoon Lee Alfred E. Glassgold 《Space Science Reviews》2000,92(1-2):153-176
We discuss the interaction between the magnetosphere of a young star and its surrounding accretion disk. We consider how an
X-wind can be driven magnetocentrifugally from the inner edge of the disk where accreting gas is diverted onto stellar field
lines either to flow onto the Sun or to be flung outwards with the wind. The X-wind satisfies many observational tests concerning
optical jets, Herbig-Haro objects, and molecular outflows. Connections may exist between primitive solar system materials
and X-winds. Chondrules and calcium-aluminum-rich inclusions (CAIs) experienced short melting events uncharacteristic of the
asteroid belt where meteorites originate. The inner edge of the solar nebula has the shortest orbital timescale available
to the system, a few days. Protosolar flares introduce another timescale, tens of minutes to hours. CAIs may form when solids
are lifted from shaded portions of the disk close to the Sun and are exposed to its intense light for a day or so before they
are flung by the X-wind to much larger distances. Chondrules were melted, perhaps many times, by flares at larger distances
from the Sun before being launched and annealed, but not remelted, in the X-wind. Aerodynamic sorting explains the narrow
range of sizes with which CAIs and chondrules are found in chondritic meteorites. Flare-generated cosmic-rays may induce spallation
reactions that produce some of the short-lived radioactivities associated with primitive solar system rocks.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
58.
Space Science Reviews - 相似文献
59.
Beginning in the early 1950s, data from neutron monitors placed the taxonomy of cosmic ray temporal variations on a firm footing,
extended the observations of the Sun as a transient source of high energy particles and laid the foundation of our early concepts
of a heliosphere. The first major impact of the arrival of the Space Age in 1957 on our understanding of cosmic rays came
from spacecraft operating beyond the confines of our magnetosphere. These new observations showed that Forbush decreases were
caused by interplanetary disturbances and not by changes in the geomagnetic field; the existence of both the predicted solar
wind and interplanetary magnetic field was confirmed; the Sun was revealed as a frequent source of energetic ions and electrons
in the 10–100 MeV range; and a number of new, low-energy particle populations was discovered. Neutron monitor data were of
great value in interpreting many of these new results.
With the launch of IMP 6 in 1971, followed by a number of other spacecraft, long-term monitoring of low and medium energy
galactic and anomalous cosmic rays and solar and interplanetary energetic particles, and the interplanetary medium were available
on a continuous basis. Many synoptic studies have been carried out using both neutron monitor and space observations. The
data from the Pioneer 10/11 and Voyagers 1/2 deep space missions and the journey of Ulysses over the region of the solar poles have significantly extended our knowledge of the heliosphere and have provided enhanced
understanding of many effects that were first identified in the neutron monitor data.
Solar observations are a special area of space studies that has had great impact on interpreting results from neutron monitors,
in particular the identification of coronal holes as the source of high-speed solar wind streams and the recognition of the
importance of coronal mass ejections in producing interplanetary disturbances and accelerating solar energetic particles.
In the future, with the new emphasis on carefully intercalibrated networks of neutron monitors and the improved instrumentation
for space studies, these symbionic relations should prove to be even more productive in extending our understanding of the
acceleration and transport of energetic particles in our heliosphere.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
60.
Space observations in several near-Earth environments have revealed the presence of positive-potential, large-amplitude electrostatic
structures, associated with high-frequency disturbances, and indicative of electron dynamics. Earlier models proposed in terms
of electron-acoustic solitary waves in a two-electron-temperature plasma were inadequate, because only negative potential
structures could thus be obtained, whereas the observations point to positive potential structures. In this paper, it is shown
that the theoretical restriction to negative potential solitons is due to the neglect of the inertia of the hot electrons,
implicitly or explicitly assumed in previous papers. If hot electron inertia is retained, however, there exists a parameter
range where positive potential solitary waves are formed, which can have important consequences for the re-interpretation
of several astrophysical phenomena involving two-electron-temperature plasmas.
PACS: 52.35.Mw, 52.35.Sb, 96.50.Ry 相似文献