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Geoffrey Andima Emirant B. Amabayo Edward Jurua Pierre J. Cilliers 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2018,61(1):264-273
Complex electrodynamic processes over the low latitude region often result in post sunset plasma density irregularities which degrade satellite communication and navigation. In order to forecast the density irregularities, their occurrence time, duration and location need to be quantified. Data from the Communication/Navigation Outage Forecasting System (C/NOFS) satellite was used to characterize the low latitude ion density irregularities from 2011 to 2013. This was supported by ground based data from the SCIntillation Network Decision Aid (SCINDA) receivers at Makerere (Geographic coordinate 32.6°E, 0.3°N, and dip latitude ?9.3°N) and Nairobi (Geographic coordinate 36.8°E, ?1.3°N, and dip latitude ?10.8°N). The results show that irregularities in ion density have a daily pattern with peaks from 20:00 to 24:00 Local Time (LT). Scintillation activity at L band and VHF over East Africa peaked in 2011 and 2012 from 20:00 to 24:00 LT, though in many cases scintillation at VHF persisted longer than that at L band. A longitudinal pattern in ion density irregularity occurrence was observed with peaks over 135–180°E and 270–300°E. The likelihood of ion density irregularity occurrence decreased with increasing altitude. Analysis of C/NOFS zonal ion drift velocities showed that the largest nighttime and daytime drifts were in 270–300°E and 300–330°E longitude regions respectively. Zonal irregularity drift velocities over East Africa were for the first time estimated from L-band scintillation indices. The results show that the velocity of plasma density irregularities in 2011 and 2012 varied daily, and hourly in the range of 50–150 m s?1. The zonal drift velocity estimates from the L-band scintillation indices had good positive correlation with the zonal drift velocities derived from VHF receivers by the spaced receiver technique. 相似文献
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186.
S.A. Elwakil M.A. Zahran E.K. El-Shewy A.E. Mowafy 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2011
A theoretical investigation has been made for adiabatic positive and negative dust charge fluctuations on the propagation of dust-ion acoustic waves (DIAWs) in a weakly inhomogeneous, collisionless, unmagnetized dusty plasmas consisting of cold positive ions, stationary positively and negatively charged dust particles and isothermal electrons. The reductive perturbation method is employed to reduce the basic set of fluid equations to the variable coefficients Korteweg–de Vries (KdV) equation. Either compressive or rarefactive solitons are shown to exist depending on the critical value of the ion density, which in turn, depends on the inhomogeneous distribution of the ion. The dissipative effects of non-adiabatic dust charge variation has been studied which cause generation of dust ion acoustic shock waves governed by KdV-Burger (KdVB) equation. The results of the present investigation may be applicable to some dusty plasma environments, such as dusty plasma existing in polar mesosphere region. 相似文献
187.
Cassini Plasma Spectrometer Investigation 总被引:1,自引:0,他引:1
《Space Science Reviews》2004,114(1-4):1-112
The Cassini Plasma Spectrometer (CAPS) will make comprehensive three-dimensional mass-resolved measurements of the full variety of plasma phenomena found in Saturn’s magnetosphere. Our fundamental scientific goals are to understand the nature of saturnian plasmas primarily their sources of ionization, and the means by which they are accelerated, transported, and lost. In so doing the CAPS investigation will contribute to understanding Saturn’s magnetosphere and its complex interactions with Titan, the icy satellites and rings, Saturn’s ionosphere and aurora, and the solar wind. Our design approach meets these goals by emphasizing two complementary types of measurements: high-time resolution velocity distributions of electrons and all major ion species; and lower-time resolution, high-mass resolution spectra of all ion species. The CAPS instrument is made up of three sensors: the Electron Spectrometer (ELS), the Ion Beam Spectrometer (IBS), and the Ion Mass Spectrometer (IMS). The ELS measures the velocity distribution of electrons from 0.6 eV to 28,250 keV, a range that permits coverage of thermal electrons found at Titan and near the ring plane as well as more energetic trapped electrons and auroral particles. The IBS measures ion velocity distributions with very high angular and energy resolution from 1 eV to 49,800 keV. It is specially designed to measure sharply defined ion beams expected in the solar wind at 9.5 AU, highly directional rammed ion fluxes encountered in Titan’s ionosphere, and anticipated field-aligned auroral fluxes. The IMS is designed to measure the composition of hot, diffuse magnetospheric plasmas and low-concentration ion species 1 eV to 50,280 eV with an atomic resolution M/ΔM ∼70 and, for certain molecules, (such asN
2
+ and CO+), effective resolution as high as ∼2500. The three sensors are mounted on a motor-driven actuator that rotates the entire instrument over approximately one-half of the sky every 3 min.This revised version was published online in July 2005 with a corrected cover date. 相似文献
188.
郭守田 《沈阳航空工业学院学报》1994,(1):59-65
不对称烯烃与不对称试剂进行亲电加成反应时,遵守马尔科夫尼可夫规则,本文从生成碳正离子和环状高价正离子的两种反应途径对其反应机理加以讨论,并指出决定两种途径的主要因素. 相似文献
189.
M. Yamauchi Y. Futaana A. Fedorov E. Dubinin R. Lundin J.-A. Sauvaud D. Winningham R. Frahm S. Barabash M. Holmstrom J. Woch M. Fraenz E. Budnik H. Borg J. R. Sharber A. J. Coates Y. Soobiah H. Koskinen E. Kallio K. Asamura H. Hayakawa C. Curtis K. C. Hsieh B. R. Sandel M. Grande A. Grigoriev P. Wurz S. Orsini P. Brandt S. Mckenna-Lawler J. Kozyra J. Luhmann 《Space Science Reviews》2006,126(1-4):239-266
Although the Mars Express (MEX) does not carry a magnetometer, it is in principle possible to derive the interplanetary magnetic
field (IMF) orientation from the three dimensional velocity distribution of pick-up ions measured by the Ion Mass Analyser
(IMA) on board MEX because pick-up ions' orbits, in velocity phase space, are expected to gyrate around the IMF when the IMF
is relatively uniform on a scale larger than the proton gyroradius. During bow shock outbound crossings, MEX often observed
cycloid distributions (two dimensional partial ring distributions in velocity phase space) of protons in a narrow channel
of the IMA detector (only one azimuth for many polar angles). We show two such examples. Three different methods are used
to derive the IMF orientation from the observed cycloid distributions. One method is intuitive (intuitive method), while the
others derive the minimum variance direction of the velocity vectors for the observed ring ions. These velocity vectors are
selected either manually (manual method) or automatically using simple filters (automatic method). While the intuitive method
and the manual method provide similar IMF orientations by which the observed cycloid distribution is well arranged into a
partial circle (representing gyration) and constant parallel velocity, the automatic method failed to arrange the data to
the degree of the manual method, yielding about a 30° offset in the estimated IMF direction. The uncertainty of the derived
IMF orientation is strongly affected by the instrument resolution. The source population for these ring distributions is most
likely newly ionized hydrogen atoms, which are picked up by the solar wind. 相似文献
190.
《中国航空学报》2020,33(12):3018-3026
The coupling region of a Hall thruster with a hollow cathode is the region between the cathode and the thruster plume. The characteristics of plasma in that region are complicated and strongly associated with the thruster working conditions and the cathode position. In this paper, a laboratory 100 W class magnetically shielded Hall thruster was coupled with a hollow cathode. Optical imaging and electrostatic probe were employed to monitor and scan the plasma plume. Plume characteristics in the coupling region in non-self-sustained mode and self-sustained mode were compared. Evolution of the coupling plume with the cathode position was studied. Experiments show that, when turning the thruster into self-sustained mode or moving the cathode further away axially, the discharge current can be reduced by 6.4–10.6% restraining the electron current and improving ionization. In particular, when the cathode is moved further, the electron conduction near the channel walls is suppressed. The electron current is reduced by 27.4% and the ion beam current is increased by 7%. Overall, this work shows that the working mode of the thruster and the position of the cathode greatly affect the coupling plasma plume. Both play an important role in improving the utilizations of propellant and current. 相似文献