Neutrinos as cluster dark matter

The dynamical mass of clusters of galaxies, calculated in terms of MOdified Newtonian Dynamics (MOND), is a factor of 2 or 3 times smaller than the Newtonian dynamical mass but remains significantly larger than the observed baryonic mass in the form of hot gas and stars in galaxies. Here I consider further the suggestion that the undetected matter might be in the form of cosmological neutrinos with mass of the order of 2 eV. If the neutrinos and baryons have comparable velocity dispersions and if the two components maintain their cosmological density ratio, then the electron density in the cores of clusters should be proportional to T ^3/2, as appears to be true in non-cooling flow clusters. This is equivalent to the 'entropy floor' proposed to explain the steepness of the observed luminosity–temperature relation, but here preheating of the medium is not required. Two-fluid (neutrino–baryon) hydrostatic models of clusters, in the context of MOND, reproduce the observed luminosity–temperature relation of clusters. If the β law is imposed on the gas density distribution, then the self-consistent models predict the general form of the observed temperature profile in both cooling and non-cooling flow clusters.     

21-cm fluctuations from inhomogeneous X-ray heating before reionization

Many models of early structure formation predict a period of heating immediately preceding reionization, when X-rays raise the gas temperature above that of the cosmic microwave background. These X-rays are often assumed to heat the intergalactic medium (IGM) uniformly, but in reality will heat the gas more strongly closer to the sources. We develop a framework for calculating fluctuations in the 21-cm brightness temperature that originate from this spatial variation in the heating rate. High-redshift sources are highly clustered, leading to significant gas temperature fluctuations (with fractional variations ∼40 per cent, peaking on   k ∼ 0.1 Mpc⁻¹  scales). This induces a distinctive peak-trough structure in the angle-averaged 21-cm power spectrum, which may be accessible to the proposed Square Kilometre Array. This signal reaches the ∼10 mK level, and is stronger than that induced by Lyα flux fluctuations. As well as probing the thermal evolution of the IGM before reionization, this 21-cm signal contains information about the spectra of the first X-ray sources. Finally, we consider disentangling temperature, density and Lyα flux fluctuations as functions of redshift.     

Evaporation and condensation of giant interstellar clouds in a hot-gas environment

Gas phases of the interstellar medium (ISM) coexist locally, penetrate each other and mix by means of dynamical and plasmaphysical processes. E.g. heat conduction from the hot to the cooler gas leads to energy and mass exchange between the gas phases. Analytical solutions exist under which evaporation of cloudy material or condensation of hot gas onto the clouds' surface dominate. Since these results are derived for stationary and static conditions and under ideal assumptions, they do not necessarily hold for a dynamical ISM. On the other hand, the mass and energy exchange between the gas phases is of great importance for the energy budget of the ISM and by this influences the evolution of galaxies. This led us to investigate the evolution of interstellar clouds in a hot gas by means of numerical simulations. At first, we compare static models with the analytical results and found that interstellar clouds with parameters requiring analytically evaporation are, in contrast, accreting surrounding material if self-gravitation and cooling are implied. For the more realistic case, where clouds are embedded in a streaming hot gas, the models show that Kelvin-Helmholtz instability which leads to the disruption of the clouds is suppressed by heat conduction so that the clouds are stabilized to survive. This revised version was published online in September 2006 with corrections to the Cover Date.     

小波变换方法在地震资料噪声消除中的应用

小波变换方法由于具有同时在时间域与频率域分析的特点,在信号的分析处理方面得到了广泛的应用,将其应用于地震信号噪声的处理,有着更好的应用前景和研究价值.笔者的研究工作主要围绕小波变换消噪过程中阈值方法的选择及阈值的选取,同时将一维小波方法与F-K滤波方法、二维小波方法与F-K方法以及这3种方法结合起来进行噪声的去除,用于实际数据处理,效果较好.     

基于电子化供应链管理的动态定价数学模型的研究

随着不确定性因素在商业交易中的越来越突出的影响，考虑价格随机波动的动态定价研究成为管理经济学的重要课题。作者把随机误差所带来的不确定因素引入制造商主导定价数学模型，引入零售价格的期望、方差和转移价格的期望，将不完全信息博弈转化为完全信息博弈，并结合最优生产和存储模型，运用泛函极值方法解决供方先动需方后动的转移价格定价问题。获得了最优转移价格的预期龙的结构模型和预期价格与价格波动的比例关系，进而指出掌握定价主动权的制造商一方掌控了大部分利润。     

Spreading of a NAPL lens in a double-porosity medium

Spreading of a non-aqueous phase liquid (NAPL) denser than water (DNAPL) lens (mound) in the unsaturated zone of double-porosity aquifer above an impervious plane boundary is investigated. The double-porosity aquifer is conceptualized as a fracture network surrounding pervious blocks. Vertical gravity equilibrium is assumed to prevail in each one of the two media, fractures and blocks. Through vertical integration, two coupled partial differential equations for the DNAPL content in each medium are obtained. The mass exchange rate between high- and low-permeability media is considered as a function of NAPL content. The dominant effect is gravity, whereas capillary forces are negligible. Analytical solutions for one-dimensional and axisymmetric problems of mound spreading are obtained.     

基于解析方法计算频散层状介质的探地雷达响应

考虑频散介质的电磁波传播,采用Cole-Cole公式建立频散模型。只考虑介质的介电常数随外加电磁场频率的变化,采用高密度采样滤波算法,模拟层状介质的雷达响应,从中可以看出频散介质对雷达波的衰减影响。     

与规范反应谱相对应的Clough-Penzien模型参数研究

根据我国现行抗震规范（GB50011—2001）的反应谱曲线，对Clough—Penzien模型的参数取值进行了具体研究。采用时间包络函数考虑地震动的非平稳性，根据加速度峰值等效原则确定了谱强度因子S0的表达式，表明谱强因子不仅与地面加速度特性、场地类别有关，而且与结构的动力特性（阻尼比、自振周期）有关。最后对谱强度因子计算做了简化处理，为随机抗震计算分析提供了参考依据。