Constraints from deuterium on the formation of icy bodies in the Jovian system and beyond

We consider the role of deuterium as a potential marker of location and ambient conditions during the formation of small bodies in our Solar system. We concentrate in particular on the formation of the regular icy satellites of Jupiter and the other giant planets, but include a discussion of the implications for the Trojan asteroids and the irregular satellites. We examine in detail the formation of regular planetary satellites within the paradigm of a circum-Jovian subnebula. Particular attention is paid to the two extreme potential subnebulae—“hot” and “cold”. In particular, we show that, for the case of the “hot” subnebula model, the D:H ratio in water ice measured from the regular satellites would be expected to be near-Solar. In contrast, satellites which formed in a “cold” subnebula would be expected to display a D:H ratio that is distinctly over-Solar. We then compare the results obtained with the enrichment regimes which could be expected for other families of icy small bodies in the outer Solar system—the Trojan asteroids and the irregular satellites. In doing so, we demonstrate how measurements by Laplace, the James Webb Space Telescope, HERSCHEL and ALMA will play an important role in determining the true formation locations and mechanisms of these objects.     

B, V, I photometry of 20 dwarf irregular galaxies within 10 Mpc

CCD photometry is presented for 20 dIrr galaxies situated in the nearby complexes CenA/M83, and CVnI as well as in the general field of the Local Volume. We present integrated magnitudes of the galaxies in   B , V , I   bands and also surface brightness profiles to a median isophote  μ _B ∼ 28  mag arcsec⁻². The popular Sersic parametrization of surface brightness profiles generally does a poor job of simultaneously fitting the inner cores and outer exponential surface brightness fall-offs observed in many of our targets. The observed sample is a part of a general project to image about 500 nearby  ( D < 10 Mpc)  dwarf galaxies in multiple bands.     

不规则波下船舶运动响应特征数值分析

针对不规则波浪作用下Wigley型船的运动响应问题进行了系统的研究,采用统计学方法深入探讨了船舶不规则运动幅值和响应周期的分布规律,并通过傅里叶变换对船舶运动响应进行了频谱特征分析。结果表明,船舶横摇方向与升沉和纵摇方向随机运动的响应特征有显著差异。在升沉与纵摇方向,波浪谱峰频率远离自振频率,前十分之一大振幅运动对应周期离散性较小,基本稳定在波浪谱峰周期附近,但小振幅运动周期分布离散性较大,频谱分析指出船舶升沉与纵摇运动响应频谱在波浪谱峰频率附近出现明显峰值。而在横摇方向,波浪谱峰频率与自振频率相耦合,不同振幅的横摇运动响应周期均稳定在自振周期附近,且周期离散性较小,频谱分析也表明横摇运动响应频谱主要集中于船舶运动自振频率附近。     

不规则网土壤测量在水系沉积物异常查证中的应用

在大兴安岭森林沼泽景观区,植被茂盛、土壤表层腐殖质发育,且通视条件差,运用传统的规则网土壤测量方法进行1/5万水系沉积物异常查证,工作周期长、劳动强度大;采用不规则网土壤测量方法进行异常查证,取得了快速评价异常、追踪异常源,缩短找矿周期的效果。     

基于GIS建立空间图形数据库的方法

数字化空间图形数据库是空间图形及其属性数据库的统，建立数字化空间图形数据库是一个非常繁琐的工程。而先建立空间图形库，然后进行各图元属性ID号排序，再“根据参数赋属性”建立完整的空间图形数据库，会取得事半功倍的效果。     

层状矿体等高线离散化后的四面体建模

基于不规则四面体的三维实体建模方法具有很多优点,但在层状矿体的建模中,该方法却不能准确地描述其层状界面。根据层状矿体建模数据的特点,先将层状矿体的等高线进行等距离散化,再建立不规则四面体三维实体模型,并为该方法设计由点、面和四面体组成的逻辑模型结构。该方法用VC++.net编程得以实现,并使用内蒙某煤矿的实际数据,建立了相应的矿床三维实体模型。实践表明,通过离散化等高线后建立的层状矿体四面体模型,能够准确反映出层状矿体的层状界面,实现对层状矿体的三维实体建模。     

二轴晶临界干涉图的发现及其消光影特征

在偏光显微镜的锥光系统中,垂直二轴品光率体─—圆切面与光轴面交线的切面干涉图此处定义为临界干涉图。结合球面和平面解析法可以证明,这种干涉图消光影一般为双曲线形,但具体形状与晶体2V角及从0°位置（光轴面平行上或下偏光镜振动方向）旋转的角度有关。它与已知其它切面干涉图的最大区别是,当晶体从0°位置旋转45°时,消光影为一条与目镜横丝或纵丝夹45°角的直线,它到视域中心的距离随晶体2V角的减小而加大,因而在特定物镜数值孔径和晶体折射率的情况下,只有较大2V角晶体的这条消光影才会处在视域之内。在观察橄榄石和角闪石晶体临界干涉图时证实了它的上述特性。     

应用Winsurf软件绘制磁场分布等值线图

观测场地磁场梯度测量结果最直观的表述方式就是利用ΔF值绘制出的场地地磁场分布等值线图。Winsurf软件是Golden公司开发的一个三维绘图软件包 ,可以绘制各种等值线图和三维立体图。目前最高版本为 8.0。本文较为详细地介绍了利用这个软件的应用方法、步骤。