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41.
42.
In this review we present the main results obtained by the ISO satellite on the abundance and spatial distribution of water
vapor in the direction of molecular clouds, evolved stars, galaxies, and in the bodies of our Solar System. We also discuss
the modeling of H2O and the difficulties found in the interpretation of the data, the need of collisional rates and the perspectives that future
high angular and high spectral resolution observations of H2O with the Herschel Space Observatory will open. 相似文献
43.
Reinhard Schlickeiser 《Space Science Reviews》1996,75(1-2):299-315
It is argued that the high-energy X-ray and -ray emission from flaring blazars is beamed radiation from the relativistic jet supporting the relativistic beaming hypothesis and the unified scenario for AGNs. Most probably the high-energy emission results from inverse Compton scattering by relativistic electrons and positrons in the jet of radiation originating external to the jet plus pair annihilation radiation from the jet. Future positive TeV detections of EGRET AGN sources will be decisive to identify the prominent target photon radiation field. Direct -ray production by energetic hadrons is not important for the flaring phase in -ray blazars, but the acceleration of energetic hadrons during the quiescent phase of AGNs is decisive as the source of secondary electrons and positrons through photo-pair and photo-pion production. Injection of ultrahigh energy secondary electrons and positrons into a stochastic quasilinear acceleration scheme during the quiescent AGN phase leads to cooling electron-positron distribution functions with a strong cut-off at low but relativistic energy that under certain local conditions may trigger a plasma instability that gives rise to an explosive event and the flaring -ray phase. 相似文献
44.
45.
Wei-Tou Ni 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2013
The detection of low frequency band (100 nHz–100 mHz) and very low frequency band (300 pHz–100 nHz) gravitational waves (GWs) is important for exploration of the equation of state of dark energy and the co-evolution of massive black holes (MBHs) with galaxies. Most galaxies are believed to have a massive black hole in the galactic core. In the formation of these black holes, merging and accretion are the two main processes. Merging of massive black holes generate GWs which could be detected by space GW detectors and Pulsar Timing Arrays (PTAs) to cosmological distances. LISA (Laser-Interferometric Space Antenna) is most sensitive to the frequency band 1 mHz–100 mHz, ASTROD-GW (ASTROD [Astrodynamical Space Test of Relativity using Optical Devices] optimized for Gravitational Wave detection) is most sensitive to the frequency band 100 nHz–1 mHz and PTAs are most sensitive to the frequency band 300 pHz–100 nHz. In this paper, we discuss the sensitivities and outlooks of detection of GWs from binary massive black holes in these frequency bands with an emphasis on ASTROD-GW. The GWs generated by the inspirals, merging and subsequent ringdowns of binary black holes are standard sirens to the cosmological distance. Using GW observations, we discuss the methods for determining the equation of state of dark energy and for testing the co-evolution models of massive black holes. ASTROD-GW is an optimization of ASTROD to focus on the goal of detection of GWs. The mission orbits of the 3 spacecraft forming a nearly equilateral triangular array are chosen to be near the Sun-Earth Lagrange points L3, L4 and L5. The 3 spacecraft range interferometrically with one another with arm length about 260 million kilometers. With 52 times longer in arm length compared to that of LISA, the strain detection sensitivity is 52 times better toward larger wavelength. The scientific aim is focused for gravitational wave detection at low frequency. The science goals include detection of GWs from MBHs, and Extreme-Mass-Ratio Black Hole Inspirals (EMRI), and using these observations to find the evolution of the equation of state of dark energy and to explore the co-evolution of massive black holes with galaxies. 相似文献
46.
S. Pellegrini L. Ciotti J.P. Ostriker 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2009
The centers of elliptical galaxies host supermassive black holes that significantly affect the surrounding interstellar medium through feedback resulting from the accretion process. The evolution of this gas and of the nuclear emission during the galaxies’ lifetime has been studied recently with high-resolution hydrodynamical simulations. These included gas cooling and heating specific for an average AGN spectral energy distribution, a radiative efficiency declining at low mass accretion rates, and mechanical coupling between the hot gas and AGN winds. Here, we present a short summary of the observational properties resulting from the simulations, focussing on (1) the nuclear luminosity; (2) the global luminosity and temperature of the hot gas; (3) its temperature profile and X-ray brightness profile. These properties are compared with those of galaxies of the local universe, pointing out the successes of the adopted feedback and the needs for new input in the simulations. 相似文献
47.
Simon Glover 《Space Science Reviews》2005,117(3-4):445-508
In this review, I survey our current understanding of how the very first stars in the universe formed, with a focus on three
main areas of interest: the formation of the first protogalaxies and the cooling of gas within them, the nature and extent
of fragmentation within the cool gas, and the physics – in particular the interplay between protostellar accretion and protostellar
feedback – that serves to determine the final stellar mass.
In each of these areas, I have attempted to show how our thinking has developed over recent years, aided in large part by
the increasing ease with which we can now perform detailed numerical simulations of primordial star formation. I have also
tried to indicate the areas where our understanding remains incomplete, and to identify some of the most important unsolved
problems. 相似文献
48.
The elliptical cross-section spiral equal-channel extrusion (ECSEE) process is simulated by using Deform-3D finite element software. The ratio m of major-axis to minor-axis length for ellipse-cross-section, the torsion angle u, the round-ellipse cross-section transitional channel L1, the elliptical rotation cross-section transitional channel L2 and the ellipse-round cross-section transitional channel L3 are destined for the extrusion process parameters. The average effective strain eave on cross-section of blank, the deformation uniformity coefficient a and the value of maximum damage dmax are chosen to be the optimize indexes, and the virtual orthogonal experiment of L16 (45) is designed. The correlation degree of the process factors affecting eave, a and dmax is analyzed by the numerical simulation results using the weights and grey association model. The process parameters are optimized by introducing the grey situation decision theory and the ECSEE optimal combination of process parameters is obtained: u of 120 , m of 1.55, L1 of 7 mm, L2 of 10 mm, and L3 of 10 mm. Simulation and experimental results show that the material can be refined with the optimized structural parameters of die. Therefore, the optimization results are satisfactory. 相似文献
49.
在交会椭圆轨道目标阶段,Hill制导受各种误差因素的影响。介绍了椭圆轨道目标Hill 制导的误差因素,并着重研究了导航误差和控制误差对终端位置的影响,给出了误差的基本 表达式。与交会圆轨道目标情况进行比较,分析了初始真近点角对导航误差引起的终端位置 偏差的影响。在此基础上给出了一种修正算法,理论上证明了修正算法能显著提高终端位置 的精度。通过Monte\|Carlo方法的仿真结果表明,合理改变初始真近点角能减小导航误差引 起的终端位置偏差,并且修正算法能更有效提高制导精度。
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50.
椭圆轨道相对动力学状态转移矩阵 总被引:1,自引:0,他引:1
针对已有研究的不足,给出了更加便于理论分析和工程应用,并具有普遍适用性的状态转移矩阵的一种新形式。基于Lawden方程推导了以三维空间中位置-速度表示的状态转移矩阵元素的具体表达式,并将其由角域变换到时域,得到了表示真实位置速度的状态转移矩阵,通过初等变换可以从该矩阵得到任意需要的形式。仿真结果表明了状态转移矩阵的有效性,可将其用于任意偏心率椭圆轨道的三维轨道交会、轨道修正、编队队形设计及控制问题。 相似文献