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491.
A. Dosch A. Shalchi 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2010
We calculate the maximum energy that a particle can obtain at perpendicular interplanetary shock waves by the mechanism of diffusive shock acceleration. The influence of the energy range spectral index of the two-dimensional modes of the interplanetary turbulence is explored. We show that changes in this parameter lead to energies that differ in at least one order of magnitude. Therefore, the large scale structure of the turbulence is a key input if the maximum particle energy is calculated. 相似文献
492.
A. Dosch A. Shalchi B. Weinhorst 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2009,44(11):2287
In the past few year several theories have been presented for describing cosmic ray scattering across the mean magnetic field. It is the purpose of the present article to discuss the relation between these different theories in order to improve our understanding of cosmic ray perpendicular scattering and to explore the parameter regimes for which these different theories are valid. 相似文献
493.
为将富油燃烧/快速淬熄/贫油燃烧(RQL)用于高温升燃烧室设计,以实现温升与排放的良好统一,对不同主燃孔位置下
的单头部矩形燃烧室流动、淬熄区气流混合、燃烧和排放特性进行数值模拟。结果表明:燃烧室中心回流区的长度和高度随着主
燃孔轴向距离的增大而增大。随着主燃孔轴向距离的增大,主燃孔射流深度增加,射流角度逐渐向下游偏转,导致淬熄区内气流
的混合效果减弱;随着主燃孔位置的后移,富油区内的当量比显著增大,导致CO和碳烟的生成量迅速增加,淬熄区内的沿程高温
区域面积逐渐缩小,燃烧效率逐渐降低。当X/H=0.7时,燃烧室沿程NO生成量始终处在较大值;而当X/H=0.9时,燃烧室沿程NO
生成量始终处于较小值,但CO的生成量增大。 相似文献
494.
A. Shalchi B. Weinhorst 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2009
One- and two-dimensional models of magnetic field fluctuations and turbulence are widely used in space-, astrophysical, and laboratory contexts. In the present article we use a generalized form of the turbulence wave spectrum to calculate field line diffusion coefficients analytically and numerically. General conditions are derived for which field line wandering behaves subdiffusively, diffusively, and superdiffusively. 相似文献
495.
利用Ansys对镀锌锅上方空间的温度场进行模拟。在模拟过程中,利用Ansys软件中的FlotranCFD模块建立模型,计算锌锅上方空间的流场和温度场分布情况,分析温度的主要影响因素,为热镀锌生产线的工程设计提供了理论依据。此方法也为温度分析提供了一种新的思路。 相似文献
496.
V.M. Dvornikov M.V. KravtsovaA.A. Lukovnikova V.E. Sdobnov 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2009
Dynamic processes in the interplanetary space have been investigated using time variations in time parameters of the cosmic-ray rigidity spectrum. Change of heliosphere electromagnetic characteristics has been found out to precede sporadic phenomena on the Sun. In particular, it is shown that sporadic phenomena are followed by generation of local polarization electric fields, decrease of the magnetic-field strength in small-scale heliospheric structures, and increase of the potential difference between the pole and the plane of the ecliptic. These features allow prediction of solar proton events in advance (from several hours to several tens of hours) with a high degree of confirmation. 相似文献
497.
Three-dimensional computational fluid dynamics analyses have been employed to study the compressible and turbulent flow of the shock train in a convergent–divergent nozzle. The primary goal is to determine the behavior, location, and number of shocks. In this context, full multi-grid initialization, Reynolds stress turbulence model (RSM), and the grid adaption techniques in the Fluent software are utilized under the 3D investigation. The results showed that RSM solution matches with the experimental data suitably. The effects of applying heat generation sources and changing inlet flow total temperature have been investigated. Our simulations showed that changes in the heat generation rate and total temperature of the intake flow influence on the starting point of shock, shock strength, minimum pressure, as well as the maximum flow Mach number. 相似文献
498.
499.
A.H. Maghrabi 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2014
Radiometric measurements of the thermal radiation originating from the moon’s surface were obtained using an infrared detector operating at wavelengths between 8 and 14 μm. The measurements cover a full moon cycle. The variation of the moon’s temperature with the lunar phase angle was established. The lunar temperatures were 391 ± 2.0 K for the full moon, 240 ± 3.5 K for the first quarter, and 236 ± 3 K for the last quarter. For the rest of the phase angles, the lunar temperature varied between 170 and 380 K. Our results are comparable with those obtained previously at these phase angles. For the new moon phase, the obtained temperature was between 120 and 133 K. With the exception of the new moon phase, our measurements at all the phase angles were consistent with those obtained using Earth-based data and those obtained by the Diviner experiment and the Clementine spacecraft. At the new phase, our measurements were comparable with those obtained from the ground but were significantly higher than those obtained by the Diviner and Clementine data. We attribute this inconsistency to either the calibration curve of our detector, which does not perform well at very low temperatures, or to infrared emission from the atmosphere. A simple linear model to predict the lunar temperature as a function of the phase angle was proposed. The experimental errors that affect the measured temperatures are discussed. 相似文献
500.
Bakul Das Shubham Sarkar Prabir Kumar Haldar Subrata Kumar Midya Sujay Pal 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2021,67(1):75-86
The D-region ionospheric disturbances due to the tropical cyclone Fani over the Indian Ocean have been analysed using Very Low Frequency (VLF) radio communication signals from three transmitters (VTX, NWC and JJI) received at two low latitude stations (Kolkata-CUB and Cooch Behar-CHB). The cyclone Fani formed from a depression on 26th April, 2019 over the Bay of Bengal (Northeastern part of the Indian Ocean) and turned into an extremely severe cyclone with maximum 1-min sustained winds of 250 km/h on 2 May, 2019 which made landfall on 3 May, 2019. Out of six propagation paths, five propagation paths, except the JJI-CHB which was far away from the cyclone track, showed strong perturbations beyond level compared to unperturbed signals. Consistent good correlations of VLF signal perturbations with the wind speed and cyclone pressure have been seen for both the receiving stations. Computations of radio signal perturbations at CUB and CHB using the Long Wave Propagation Capability (LWPC) code revealed a Gaussian perturbation in the D-region ionosphere. Analysis of atmospheric temperature at different layers from the NASA’s TIMED satellite revealed a cooling effect near the tropopause and warming effects near the stratopause and upper mesosphere regions on 3 May, 2019. This study shows that the cyclone Fani perturbed the whole atmosphere, from troposphere to ionosphere and the VLF waves responded to the disturbances in the conductivity profiles of the lower ionosphere. 相似文献