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21.
C.L. Stokely E.G. Stansbery R.M. Goldstein 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2009
The continual monitoring of the low Earth orbit (LEO) debris environment using highly sensitive radars is essential for an accurate characterization of these dynamic populations. Debris populations are continually evolving since there are new debris sources, previously unrecognized debris sources, and debris loss mechanisms that are dependent on the dynamic space environment. Such radar data are used to supplement, update, and validate existing orbital debris models. NASA has been utilizing radar observations of the debris environment for over a decade from three complementary radars: the NASA JPL Goldstone radar, the MIT Lincoln Laboratory (MIT/LL) Long Range Imaging Radar (known as the Haystack radar), and the MIT/LL Haystack Auxiliary radar (HAX). All of these systems are highly sensitive radars that operate in a fixed staring mode to statistically sample orbital debris in the LEO environment. Each of these radars is ideally suited to measure debris within a specific size region. The Goldstone radar generally observes objects with sizes from 2 mm to 1 cm. The Haystack radar generally measures from 5 mm to several meters. The HAX radar generally measures from 2 cm to several meters. These overlapping size regions allow a continuous measurement of cumulative debris flux versus diameter from 2 mm to several meters for a given altitude window. This is demonstrated for all three radars by comparing the debris flux versus diameter over 200 km altitude windows for 3 nonconsecutive years from 1998 to 2003. These years correspond to periods before, during, and after the peak of the last solar cycle. Comparing the year to year flux from Haystack for each of these altitude regions indicate statistically significant changes in subsets of the debris populations. Potential causes of these changes are discussed. These analysis results include error bars that represent statistical sampling errors. 相似文献
22.
We present results from hybrid (particle ions, fluid electrons) simulations of the evolution of Alfvén waves close to the
ion cyclotron frequency in the solar wind, which take into account the basic properties of the background solar wind flow,
i.e., the spherical expansion and the consequent decrease in magnetic field and cyclotron frequency with increasing distance
from the Sun. We follow the evolution of a plasma parcel in a frame of reference moving with the solar wind using a 1D expanding
box hybrid model; use of the hybrid model yields a fully self-consistent treatment of the resonant cyclotron wave-particle
interaction. This model is related to a previous MHD model (Velli et al. 1992), which allows the use of a simple Cartesian
geometry with periodic boundary conditions. The use of stretched expanding coordinates in directions transverse to the mean
radial solar wind flow naturally introduces an anisotropic damping effect on velocity and magnetic field. We present results
for the case of a single circularly polarized Alfvén wave propagating radially outward. Initially, the wave is below the cyclotron
frequency for both the alpha partcles and protons. As the wind expands, the wave frequency (as seen in the solar wind frame)
decreases more slowly than the cyclotron frequencies and the wave comes into resonance. With only protons, heating occurs
as the wave frequency approaches the proton cyclotron frequency. With both alphas and protons, the alphas, which come into
resonance first, are observed to be preferentially heated and accelerated.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
23.
J. Goldstein 《Space Science Reviews》2006,124(1-4):203-216
The plasmasphere is the cold, dense innermost region of the magnetosphere that is populated by upflow of ionospheric plasma
along geomagnetic field lines. Driven directly by dayside magnetopause reconnection, enhanced sunward convection erodes the
outer layers of the plasmasphere. Erosion causes the plasmasphere outer boundary, the plasmapause, to move inward on the nightside
and outward on the dayside to form plumes of dense plasma extending sunward into the outer magnetosphere. Coupling between
the inner magnetosphere and ionosphere can significantly modify the convection field, either enhancing sunward flows near
dusk or shielding them on the night side. The plasmaspheric configuration plays a crucial role in the inner magnetosphere;
wave-particle interactions inside the plasmasphere can cause scattering and loss of warmer space plasmas such as the ring
current and radiation belts. 相似文献
24.
J. L. Burch R. Goldstein T. E. Cravens W. C. Gibson R. N. Lundin C. J. Pollock J. D. Winningham D. T. Young 《Space Science Reviews》2007,128(1-4):697-712
The ion and electron sensor (IES) is part of the Rosetta Plasma Consortium (RPC). The IES consists of two electrostatic plasma
analyzers, one each for ions and electrons, which share a common entrance aperture. Each analyzer covers an energy/charge
range from 1 eV/e to 22 keV/e with a resolution of 4%. Electrostatic deflection is used at the entrance aperture to achieve
a field of view of 90°× 360° (2.8π sr). Angular resolution is 5°× 22.5° for electrons and 5°× 45° for ions with the sector
containing the solar wind being further segmented to 5°× 5°. The three-dimensional plasma distributions obtained by IES will
be used to investigate the interaction of the solar wind with asteroids Steins and Lutetia and the coma and nucleus of comet
67P/Churyumov–Gerasimenko (CG). In addition, photoelectron spectra obtained at these bodies will help determine their composition. 相似文献
25.
H. E. Spence G. D. Reeves D. N. Baker J. B. Blake M. Bolton S. Bourdarie A. A. Chan S. G. Claudepierre J. H. Clemmons J. P. Cravens S. R. Elkington J. F. Fennell R. H. W. Friedel H. O. Funsten J. Goldstein J. C. Green A. Guthrie M. G. Henderson R. B. Horne M. K. Hudson J.-M. Jahn V. K. Jordanova S. G. Kanekal B. W. Klatt B. A. Larsen X. Li E. A. MacDonald I. R. Mann J. Niehof T. P. O’Brien T. G. Onsager D. Salvaggio R. M. Skoug S. S. Smith L. L. Suther M. F. Thomsen R. M. Thorne 《Space Science Reviews》2013,179(1-4):311-336
26.
R. Goldstein M.M. Neugebauer 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》1982,2(10):271-281
Magnetic and RF mass spectrometers have been used routinely in ionospheric research, while traditional ionospheric, magnetospheric, and interplanetary plasma measurements have been made with several types of electrostatic analyzers. Proper interpretation of these data is possible if the spectral peaks are well defined, although ambiguities between fast, light ions and slow, heavy ions cannot always be satisfactorily resolved. Recent and planned experiments involve the study of plasmas which are sufficiently energetic that the spectral peaks overlap. Furthermore, these studies of ionosphere/magnetosphere coupling and of the interaction of the solar wind with the atmospheres of Venus and comets require unambiguous identification of the ion masses with simultaneous mapping of the three-dimensional velocity distribution function of each ion species. This challenge has been partially met by several new types of instruments; the two most common types involve either (1) sequential electrostatic and magnetic analyses or (2) sequential electrostatic and time-of-flight analyses. Some new instruments have also incorporated measurements of total kinetic energy, electric charge, or secondary emission coefficients as diagnostic tools. This paper reviews these recent advances and points out areas where further development is expected and needed. 相似文献
27.
28.
Suess S. T. Phillips J. L. McComas D. J. Goldstein B. E. Neugebauer M. Nerney S. 《Space Science Reviews》1998,83(1-2):75-86
The solar wind in the inner heliosphere, inside ~ 5 AU, has been almost fully characterized by the addition of the high heliographic latitude Ulysses mission to the many low latitude inner heliosphere missions that preceded it. The two major omissions are the high latitude solar wind at solar maximum, which will be measured during the second Ulysses polar passages, and the solar wind near the Sun, which could be analyzed by a Solar Probe mission. Here, existing knowledge of the global solar wind in the inner heliosphere is summarized in the context of the new results from Ulysses. 相似文献
29.
D. T. Young J. E. Nordholt J. L. Burch D. J. McComas R. P. Bowman R. A. Abeyta J. Alexander J. Baldonado P. Barker R. K. Black T. L. Booker P. J. Casey L. Cope F. J. Crary J. P. Cravens H. O. Funsten R. Goldstein D. R. Guerrero S. F. Hahn J. J. Hanley B. P. Henneke E. F. Horton D. J. Lawrence K. P. McCabe D. Reisenfeld R. P. Salazar M. Shappirio S. A. Storms C. Urdiales J. H. Waite Jr. 《Space Science Reviews》2007,129(4):327-357
The Plasma Experiment for Planetary Exploration (PEPE) flown on Deep Space 1 combines an ion mass spectrometer and an electron
spectrometer in a single, low-resource instrument. Among its novel features PEPE incorporates an electrostatically swept field-of-view
and a linear electric field time-of-flight mass spectrometer. A significant amount of effort went into developing six novel
technologies that helped reduce instrument mass to 5.5 kg and average power to 9.6 W. PEPE’s performance was demonstrated
successfully by extensive measurements made in the solar wind and during the DS1 encounter with Comet 19P/Borrelly in September
2001.
P. Barker is deceased. 相似文献
30.
C. Carr E. Cupido C. G. Y. Lee A. Balogh T. Beek J. L. Burch C. N. Dunford A. I. Eriksson R. Gill K. H. Glassmeier R. Goldstein D. Lagoutte R. Lundin K. Lundin B. Lybekk J. L. Michau G. Musmann H. Nilsson C. Pollock I. Richter J. G. Trotignon 《Space Science Reviews》2007,128(1-4):629-647
The Rosetta Plasma Consortium (RPC) will make in-situ measurements of the plasma environment of comet 67P/Churyumov-Gerasimenko.
The consortium will provide the complementary data sets necessary for an understanding of the plasma processes in the inner
coma, and the structure and evolution of the coma with the increasing cometary activity. Five sensors have been selected to
achieve this: the Ion and Electron Sensor (IES), the Ion Composition Analyser (ICA), the Langmuir Probe (LAP), the Mutual
Impedance Probe (MIP) and the Magnetometer (MAG). The sensors interface to the spacecraft through the Plasma Interface Unit
(PIU). The consortium approach allows for scientific, technical and operational coordination, and makes optimum use of the
available mass and power resources. 相似文献