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671.
O'Sullivan J.A. DeVore M.D. Kedia V. Miller M.I. 《IEEE transactions on aerospace and electronic systems》2001,37(1):91-108
A family of conditionally Gaussian signal models for synthetic aperture radar (SAR) imagery is presented, extending a related class of models developed for high resolution radar range profiles. This signal model is robust with respect to the variations of the complex-valued radar signals due to the coherent combination of returns from scatterers as those scatterers move through relative distances on the order of a wavelength of the transmitted signal (target speckle). The target type and the relative orientations of the sensor, target, and ground plane parameterize the conditionally Gaussian model. Based upon this model, algorithms to jointly estimate both the target type and pose are developed. Performance results for both target pose estimation and target recognition are presented for publicly released data from the MSTAR program 相似文献
672.
T. Van Doorsselaere I. Arregui J. Andries M. Goossens S. Poedts 《Space Science Reviews》2005,121(1-4):79-89
We will discuss the observed, heavily damped transversal oscillations of coronal loops. These oscillations are often modeled as transversal kink oscillations in a cylinder. Several features are added to the classical cylindrical model. In our models we include loop curvature, longitudinal density stratification, and highly inhomogeneous radial density profiles. In this paper, we will first give an overview of recently obtained results, both analytically and numerically. After that, we shed a light on the computational aspects of the modeling process. In particular, we will focus on the parallellization of the numerical codes. 相似文献
673.
D. B. Reisenfeld D. S. Burnett R. H. Becker A. G. Grimberg V. S. Heber C. M. Hohenberg A. J. G. Jurewicz A. Meshik R. O. Pepin J. M. Raines D. J. Schlutter R. Wieler R. C. Wiens T. H. Zurbuchen 《Space Science Reviews》2007,130(1-4):79-86
Analysis of the Genesis samples is underway. Preliminary elemental abundances based on Genesis sample analyses are in good
agreement with in situ-measured elemental abundances made by ACE/SWICS during the Genesis collection period. Comparison of
these abundances with those of earlier solar cycles indicates that the solar wind composition is relatively stable between
cycles for a given type of flow. ACE/SWICS measurements for the Genesis collection period also show a continuum in compositional
variation as a function of velocity for the quasi-stationary flow that defies the simple binning of samples into their sources
of coronal hole (CH) and interstream (IS). 相似文献
674.
Phenneger M. Woodward J. Cox R. Gliniak C. 《Aerospace and Electronic Systems Magazine, IEEE》2008,23(7):4-4
This describes a NOAA-14 spacecraft loss of control event and the lessons learned. The lessons learned are in two categories: contingency recovery operations; and on-orbit propulsion system isolation methods. The work is motivated in recognition of the effort of the NOAA off-line engineering support team and their NOAA civil servant mission leads and operations support staff. 相似文献
675.
Leslie A. Young S. Alan Stern Harold A. Weaver Fran Bagenal Richard P. Binzel Bonnie Buratti Andrew F. Cheng Dale Cruikshank G. Randall Gladstone William M. Grundy David P. Hinson Mihaly Horanyi Donald E. Jennings Ivan R. Linscott David J. McComas William B. McKinnon Ralph McNutt Jeffery M. Moore Scott Murchie Catherine B. Olkin Carolyn C. Porco Harold Reitsema Dennis C. Reuter John R. Spencer David C. Slater Darrell Strobel Michael E. Summers G. Leonard Tyler 《Space Science Reviews》2008,140(1-4):93-127
The New Horizons spacecraft will achieve a wide range of measurement objectives at the Pluto system, including color and panchromatic maps, 1.25–2.50 micron spectral images for studying surface compositions, and measurements of Pluto’s atmosphere (temperatures, composition, hazes, and the escape rate). Additional measurement objectives include topography, surface temperatures, and the solar wind interaction. The fulfillment of these measurement objectives will broaden our understanding of the Pluto system, such as the origin of the Pluto system, the processes operating on the surface, the volatile transport cycle, and the energetics and chemistry of the atmosphere. The mission, payload, and strawman observing sequences have been designed to achieve the NASA-specified measurement objectives and maximize the science return. The planned observations at the Pluto system will extend our knowledge of other objects formed by giant impact (such as the Earth–moon), other objects formed in the outer solar system (such as comets and other icy dwarf planets), other bodies with surfaces in vapor-pressure equilibrium (such as Triton and Mars), and other bodies with N2:CH4 atmospheres (such as Titan, Triton, and the early Earth). 相似文献
676.
V. Florinski A. Balogh J. R. Jokipii D. J. McComas M. Opher N. V. Pogorelov J. D. Richardson E. C. Stone B. E. Wood 《Space Science Reviews》2009,143(1-4):57-83
Properties of the heliospheric interface, a complex product of an interaction between charged and neutral particles and magnetic fields in the heliosphere and surrounding Circumheliospheric Medium, are far from being fully understood. Recent Voyager spacecraft encounters with the termination shock and their observations in the heliosheath revealed multiple energetic particle populations and noticeable spatial asymmetries not accounted for by the classic theories. Some of the challenges still facing space physicists include the origin of anomalous cosmic rays, particle acceleration downstream of the termination shock, the role of interstellar magnetic fields in producing the global asymmetry of the interface, the influence of charge exchange and interstellar neutral atoms on heliospheric plasma flows, and the signatures of solar magnetic cycle in the heliosheath. These and other outstanding issues are reviewed in this joint report of working groups 4 and 6. 相似文献
677.
Mahaffy P.R. Donahue T.M. Atreya S.K. Owen T.C. Niemann H.B. 《Space Science Reviews》1998,84(1-2):251-263
The Galileo Probe Mass Spectrometer measurements in the atmosphere of Jupiter give D/H = (2.6 ± 0.7) × 10-5 3He/4He = (1.66 ± 0.05) × 10-4These ratios supercede earlier results by Niemann et al. (1996) and are based on a reevaluation of the instrument response at high count rates and a more detailed study of the contributions of different species to the mass peak at 3 amu. The D/H ratio is consistent with Voyager and ground based data and recent spectroscopic and solar wind (SW) values obtained from the Infrared Spectroscopic Observatory (ISO) and Ulysses. The 3He/4He ratio is higher than that found in meteoritic gases (1.5 ± 0.3) × 10-4. The Galileo result for D/H when compared with that for hydrogen in the local interstellar medium (1.6 ± 0.12) × 10-5 implies a small decrease in D/H in this part of the universe during the past 4.55 billion years. Thus, it tends to support small values of primordial D/H - in the range of several times 10-5 rather than several times 10-4. These results are also quite consistent with no change in (D+3He)/H during the past 4.55 billion years in this part of our galaxy. 相似文献
678.
Expressions for moving target indicator (MTI) improvement factor limitation due to pulse repetition frequency (PRF) staggering and loss of target detectability for various values of Doppler frequency in the passband are presented. It is also shown that the product of variance of stagger periods and clutter variance is an important parameter determining the performance of a staggered PRF MTI radar. 相似文献
679.
A. L. Broadfoot B. R. Sandel D. E. Shemansky S. K. Atreya T. M. Donahue H. W. Moos J. L. Bertaux J. E. Blamont J. M. Ajello D. F. Strobel J. C. McConnell A. Dalgarno R. Goody M. B. McElroy Y. L. Yung 《Space Science Reviews》1977,21(2):183-205
The Voyager Ultraviolet Spectrometer (UVS) is an objective grating spectrometer covering the wavelength range of 500–1700 Å with 10 Å resolution. Its primary goal is the determination of the composition and structure of the atmospheres of Jupiter, Saturn, Uranus and several of their satellites. The capability for two very different observational modes have been combined in a single instrument. Observations in the airglow mode measure radiation from the atmosphere due to resonant scattering of the solar flux or energetic particle bombardment, and the occultation mode provides measurements of the atmospheric extinction of solar or stellar radiation as the spacecraft enters the shadow zone behind the target. In addition to the primary goal of the solar system atmospheric measurements, the UVS is expected to make valuable contributions to stellar astronomy at wavelengths below 1000 Å. 相似文献
680.
J. Wicht M. Mandea F. Takahashi U. R. Christensen M. Matsushima B. Langlais 《Space Science Reviews》2007,132(2-4):261-290
Mariner 10 measurements proved the existence of a large-scale internal magnetic field on Mercury. The observed field amplitude,
however, is too weak to be compatible with typical convective planetary dynamos. The Lorentz force based on an extrapolation
of Mariner 10 data to the dynamo region is 10−4 times smaller than the Coriolis force. This is at odds with the idea that planetary dynamos are thought to work in the so-called
magnetostrophic regime, where Coriolis force and Lorentz force should be of comparable magnitude. Recent convective dynamo
simulations reviewed here seem to resolve this caveat. We show that the available convective power indeed suffices to drive
a magnetostrophic dynamo even when the heat flow though Mercury’s core–mantle boundary is subadiabatic, as suggested by thermal
evolution models. Two possible causes are analyzed that could explain why the observations do not reflect a stronger internal
field. First, toroidal magnetic fields can be strong but are confined to the conductive core, and second, the observations
do not resolve potentially strong small-scale contributions. We review different dynamo simulations that promote either or
both effects by (1) strongly driving convection, (2) assuming a particularly small inner core, or (3) assuming a very large
inner core. These models still fall somewhat short of explaining the low amplitude of Mariner 10 observations, but the incorporation
of an additional effect helps to reach this goal: The subadiabatic heat flow through Mercury’s core–mantle boundary may cause
the outer part of the core to be stably stratified, which would largely exclude convective motions in this region. The magnetic
field, which is small scale, strong, and very time dependent in the lower convective part of the core, must diffuse through
the stagnant layer. Here, the electromagnetic skin effect filters out the more rapidly varying high-order contributions and
mainly leaves behind the weaker and slower varying dipole and quadrupole components (Christensen in Nature 444:1056–1058,
2006). Messenger and BepiColombo data will allow us to discriminate between the various models in terms of the magnetic fields
spatial structure, its degree of axisymmetry, and its secular variation. 相似文献