自动剔除速度谱数据野值的方法

速度谱数据中通常存在野值,剔队其野值可提高速度谱数据的精度和可靠性,有利于实际利用。作者在文中引入数理统计方法中的Ｇｒｕｂｂｓ法和ｔ检验法,并将此二法各自的优点结合起来判野值,然后剔除。实际应用表明,效果是明显的。     

关于矿产资源储量数据库的思考

阐述了矿产资源 /储量数据库入库单元选择的合理性 ;提出了资源 /储量核算应以入库单元为基本单元 ;指出了数据库在满足资源 /储量统计工作中的需要 ,反映了矿产资源 /储量实体关系方面存在的一些问题 ,并提出了具体的解决方法。     

河北蔚县崔家寨井田构造复杂程度定量评价

地质构造复杂程度定量评价是当前矿井地质工作的研究热点之一,其关键技术体现在评价指标和评价数学模型两方面。在地质分析和勘探资料处理的基础上,选取5个非连续性变形参数和5个连续性变形参数,作为地质构造复杂性评价的指标,分别采用统计综合评价和模糊综合评价数学模型,对冀西北蔚县矿区崔家寨井田主采煤层的构造复杂程度进行定量评价,取得良好效果。对比分析表明,两种评价模型在矿井构造复杂程度定量评价方面各有优劣,比较而言,模糊综合评价模型更加客观合理。      

路基下岩溶稳定性评价的模糊多层次多属性决策方法研究

影响高速公路路基下岩溶稳定性的因素很多,影响程度各不相同且包含各种模糊信息。基于实际工程资料,综合运用层次分析方法和模糊多属性决策方法,建立路基下岩溶顶板稳定性评价的模糊多层次多属性决策模型;采用Laagoven和Buckley关于层次分析方法中权重比矩阵元素模糊化的建议,推导出权重比矩阵元素为三角模糊数的模糊权值向量计算公式,再按照模糊平均加权方法（F-SAW）得到每个评语的模糊效应值;最后以此结果进行模糊集排序,得到岩溶顶板稳定性的评语。实际工程的应用结果表明了方法的可行性和有效性,为岩溶区路基稳定性评价提供了新的思路和方法。     

荒漠绿洲防风固沙林体系的模糊综合评判——以高台县为例

运用模糊数学方法,以植物生长状况及固沙效果、土壤机械组成和土壤含水量3类指标对高台沙区现存的、定植20 a后的7种防风固沙林配置类型综合评判后,认为花棒+柠条锦鸡儿+梭梭（6 m×3 m）的隔带混交类型、梭梭+花棒（4.5 m×3 m）的隔带混交类型及柠条锦鸡儿(6 m×5 m)为生态健康,综合效益好,可以在高台沙区推广应用。     

The bimodal spiral galaxy surface brightness distribution

We have assessed the significance of Tully and Verheijen's bimodal Ursa Major Cluster spiral galaxy near-infrared surface brightness distribution, focusing on whether this bimodality is simply an artefact of small number statistics. A Kolmogorov–Smirnov style of significance test shows that the total distribution is fairly represented by a single-peaked distribution, but that their isolated galaxy subsample (with no significant neighbours within a projected distance of ∼80 kpc) is bimodal at the 96 per cent level. We have also investigated the assumptions underlying the isolated galaxy surface brightness distribution, finding that the (often large) inclination corrections used in the construction of this distribution reduce the significance of the bimodality. We conclude that the Ursa Major Cluster data set is insufficient to establish the presence of a bimodal near-infrared surface brightness distribution: an independent sample of ∼100 isolated, low-inclination galaxies is required to establish bimodality at the 99 per cent level.     

Gravitational lensing by elliptical galaxies

The fraction of high-redshift sources which are multiply imaged by intervening galaxies is strongly dependent on the cosmological constant, and so can be a useful probe of the cosmological model. However its power is limited by various systematic (and random) uncertainties in the calculation of lensing probabilities, one of the most important of which is the dynamical normalization of elliptical galaxies. Assuming ellipticals' mass distributions can be modelled as isothermal spheres, the mass normalization depends on the velocity anisotropy, the luminosity density, the core radius and the area over which the velocity dispersion is measured. The differences in the lensing probability and optical depth produced by using the correct normalization can be comparable to the differences between even the most extreme cosmological models. The existing data are not sufficient to determine the correct normalization with enough certainty to allow lensing statistics to be used to their full potential. However, as the correct lensing probability is almost certainly higher than is usually assumed, upper bounds on the cosmological constant are not weakened by these possibilities.     

Intrinsic correlation of galaxy shapes: implications for weak lensing measurements

Weak gravitational lensing is now established as a powerful method to measure mass fluctuations in the universe. It relies on the measurement of small coherent distortions of the images of background galaxies. Even low-level correlations in the intrinsic shapes of galaxies could however produce a significant spurious lensing signal. These correlations are also interesting in their own right, since their detection would constrain models of galaxy formation. Using     haloes found in N -body simulations, we compute the correlation functions of the intrinsic ellipticity of spiral galaxies assuming that the disc is perpendicular to the angular momentum of the dark matter halo. We also consider a simple model for elliptical galaxies, in which the shape of the dark matter halo is assumed to be the same as that of the light. For deep lensing surveys with median redshifts ∼1, we find that intrinsic correlations of ∼10⁻⁴ on angular scales     are generally below the expected lensing signal, and contribute only a small fraction of the excess signals reported on these scales. On larger scales we find limits to the intrinsic correlation function at a level ∼10⁻⁵, which gives a (model-dependent) range of separations for which the intrinsic signal is about an order of magnitude below the ellipticity correlation function expected from weak lensing. Intrinsic correlations are thus negligible on these scales for dedicated weak lensing surveys. For wider but shallower surveys such as SuperCOSMOS, APM and SDSS, we cannot exclude the possibility that intrinsic correlations could dominate the lensing signal. We discuss how such surveys could be used to calibrate the importance of this effect, as well as study spin–spin correlations of spiral galaxies.     

Projected bispectrum in spherical harmonics and its application to angular galaxy catalogues

We present a theoretical and exact analysis of the bispectrum of projected galaxy catalogues. The result can be generalized to evaluate the projection in spherical harmonics of any 3D bispectrum and therefore has applications to cosmic microwave background and gravitational lensing studies.
By expanding the 2D distribution of galaxies on the sky in spherical harmonics, we show how the three-point function of the coefficients can be used in principle to determine the bias parameter of the galaxy sample. If this can be achieved, it would allow a lifting of the degeneracy between the bias and the matter density parameter of the Universe, which occurs in linear analysis of 3D galaxy catalogues. In previous papers, we have shown how a similar analysis can be done in three dimensions, and we show here through an error analysis and by implementing the method on a simulated projected catalogue that ongoing three-dimensional galaxy redshift surveys (even with all the additional uncertainties introduced by partial sky coverage, redshift-space distortions and smaller numbers) will do far better than all-sky projected catalogues with similar selection function.     

可控阵的图论特征

文中提出了模糊矩阵有向图的强链的概念 ,并利用它对可控阵的图进行了研究 ,揭示可控阵的有向图中无强圈的特征 ;着重讨论可控阵的可控度 ,给出可控度的强链刻画。在此基础上 ,通过可控度的性质及其与可控阵、可控阵的标准型的关系研究 ,得出可控度为图中最长强链的长度加 1和可控阵的周期≤ 2的结果。