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Janusz Mlynarczyk Piotr Koperski Andrzej Kulak 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2012,49(1):83-88
The Digital Radio Mondiale (DRM), one of the new digital radio broadcasting standards, has been designed to overcome typical short wave radio channel difficulties, such as the multipath propagation and fast temporal changes of the received signal level, both related to the properties of the ionosphere along the path of propagation. In particular, some of the RF carriers used in the applied COFDM transmission technique serve to estimate the current state of the radio channel to enable the proper demodulation of the received signal.We have been detecting such RF carriers on select frequency channels (standard DRM broadcast) using a network of recording stations located in different parts of Poland in order to collect data on the HF radio channel. We have been also evaluating the usefulness of this procedure in providing information on the current state of the ionosphere in the refraction region between the transmitter and receivers. When the DRM system becomes more widespread, this method can supplement data that comes from the ionosondes, since it does not require much financial resources and the receivers can be easily scattered over a large area. This paper presents a set of experimental data and its analysis. 相似文献
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Andrzej Pilatowicz 《Space Science Reviews》1983,35(1):43-48
The main results of radio noise measurements taken in Poland for 220 and 400 kV power lines are presented. The influence of various line parameters, such as conductor diameter and number, phase spacing, and height of conductor above ground on the radio noise level for power lines is discussed. The basic philosophy of choosing the line parameters and route at the design stage in Poland is described taking into account radio noise levels, electrical field gradients, and corona losses. 相似文献
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Leszek Czechowski 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2009
The ‘traditional’ formulas giving the Nusselt number Nu as a function of Rayleigh number Ra cannot be used for low and moderate values of Ra. Moreover, the recent progress in 3D numerical modeling makes possible to determine the Nusselt number Nu as a function of Rayleigh number Ra for convection driven by radiogenic and tidal heating. We found that for low and moderate Ra: Nu(Ra) = ε(Ra+ξ)λ where λ depends on rheology and boundary conditions, ε depends only on the mode of heating, and ξ = ε−1/λ · Nu(Ra) makes possible to develop a parameterized theory of convection in medium size icy satellites. We also indicate some differences between convection driven by tidal and radiogenic heating and convection driven exclusively by radiogenic heating. 相似文献
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W. I. Axford J. F. McKenzie G. V. Sukhorukova M. Banaszkiewicz A. Czechowski R. Ratkiewicz 《Space Science Reviews》1999,87(1-2):25-41
We outline a theory for the origin and acceleration of the fast solar wind as a consequence of network microflares releasing
a spectrum of high frequency Alfvén waves which heat (by cyclotron absorption) the corona close to the Sun. The significant
features of our model of the fast wind are that the acceleration is rapid with the sonic point at around two solar radii,
the proton temperatures are high (~ 5 million degrees) and the minor ions are correspondingly hotter, roughly in proportion
to their mass. Moreover we argue that since the energy flux needed to power the quiet corona in closed field regions is about
the same as that needed to drive the fast solar wind, and also because at deeper levels (< 2 × 105 K) there is no great difference in the properties of supergranules and network in closed and open field regions, the heating
process (i.e., dissipation of high frequency waves) must be the same in both cases.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
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Andrzej Tomczyk 《Aerospace Science and Technology》2005,9(8):692-700
The handling qualities of an aircraft will be improved if the Direct Lift Control (DLC) system is applied. In this paper, an attempt has been made to evaluate the influence of DLC-type system parameters on the aircraft's maneuverability and to determine the desired values of these parameters for the purpose of obtaining required values of the handling maneuverability criteria. Published papers which deal with direct lift control do not list requirements for evaluating handling qualities and maneuverability of aircraft equipped with DLC system. In this paper, three new criteria permitting the evaluation of results of employing DLC have been defined. Analysis of influence of DLC system parameters on selected known handling qualities criteria (for example CAP, C*), as well as new DLC efficiency coefficients, have been illustrated with a numeric example of A4D “Skyhawk” fighter aircraft and PZL M-18 “Dromader” agricultural airplane control system modification. 相似文献
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Lasek Andrzej Brun Edmond Antoine 《IEEE transactions on aerospace and electronic systems》1967,(3):460-464
An attempt to employ a magnetically driven shock tube as a tool for aerodynamic studies of high velocity and high enthalpy flows is described. Examples of results are given. 相似文献
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N. V. Pogorelov H. Fichtner A. Czechowski A. Lazarian B. Lembege J. A. le Roux M. S. Potgieter K. Scherer E. C. Stone R. D. Strauss T. Wiengarten P. Wurz G. P. Zank M. Zhang 《Space Science Reviews》2017,212(1-2):193-248
This paper summarizes the results obtained by the team “Heliosheath Processes and the Structure of the Heliopause: Modeling Energetic Particles, Cosmic Rays, and Magnetic Fields” supported by the International Space Science Institute (ISSI) in Bern, Switzerland. We focus on the physical processes occurring in the outer heliosphere, especially at its boundary called the heliopause, and in the local interstellar medium. The importance of magnetic field, charge exchange between neutral atoms and ions, and solar cycle on the heliopause topology and observed heliocentric distances to different heliospheric discontinuities are discussed. It is shown that time-dependent, data-driven boundary conditions are necessary to describe the heliospheric asymmetries detected by the Voyager spacecraft. We also discuss the structure of the heliopause, especially due to its instability and magnetic reconnection. It is demonstrated that the Rayleigh–Taylor instability of the nose of the heliopause creates consecutive layers of the interstellar and heliospheric plasma which are magnetically connected to different sources. This may be a possible explanation of abrupt changes in the galactic and anomalous cosmic ray fluxes observed by Voyager 1 when it was crossing the heliopause structure for a period of about one month in the summer of 2012. This paper also discusses the plausibility of fitting simulation results to a number of observational data sets obtained by in situ and remote measurements. The distribution of magnetic field in the vicinity of the heliopause is discussed in the context of Voyager measurements. It is argued that a classical heliospheric current sheet formed due to the Sun’s rotation is not observed by in situ measurements and should not be expected to exist in numerical simulations extending to the boundary of the heliosphere. Furthermore, we discuss the transport of energetic particles in the inner and outer heliosheath, concentrating on the anisotropic spatial diffusion diffusion tensor and the pitch-angle dependence of perpendicular diffusion and demonstrate that the latter can explain the observed pitch-angle anisotropies of both the anomalous and galactic cosmic rays in the outer heliosheath. 相似文献
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L. Czechowski J. Leliwa-Kopystyński 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2008
Images from the Cassini mission show the existence of a long ridge on Iapetus. It extends at least 1400 km along the great circle defined by the equator. We discuss the possibility that the ridge is a result of extensional forces acting above an ascending current of solid-state convection. A two-cell pattern of convection is a reasonable explanation of the observed feature. Three scenarios of the ridge formation are proposed: spin–orbit resonance scenario, convection in low viscosity-interior scenario, and impact generating flow scenario. 相似文献
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