A New Machine for Planarity Measurement of CCDs and Mosaics of CCDs

High quality CCD detectors are now being produced with 2048× 4096 square pixels, each 15 m on a side. Evenlarger detector areas are built with several CCDs mounted into amosaic. To be useful in an instrument the light must be in focuson all CCDs, requiring that all CCDs in a mosaic must typicallybe aligned within 30 micron of a flat plane. To achieve thisaccuracy in many cases the measurement and correction of the CCDalignment is necessary. One way allowing a surface measurement,even when the CCD is protected by a window, is to usetriangulation sensor. The principle of a triangulation sensor,its application and its implementation in a measuring machineare presented here.     

A new method to derive star formation histories of galaxies from their star cluster distributions

Star formation happens in a clustered way which is why the star cluster population of a particular galaxy is closely related to the star formation history of this galaxy. From the probabilistic nature of a mass function follows that the mass of the most massive cluster of a complete population, M _max, has a distribution with the total mass of the population as a parameter. The total mass of the population is connected to the star formation rate (SFR) by the length of a formation epoch.
Since due to evolutionary effects only massive star clusters are observable up to high ages, it is convenient to use this M _max(SFR) relation for the reconstruction of a star formation history. The age distribution of the most massive clusters can therefore be used to constrain the star formation history of a galaxy. The method, including an assessment of the inherent uncertainties, is introduced with this contribution, while following papers will apply this method to a number of galaxies.     

Star formation in a multi-phase interstellar medium

This contribution reports on our first efforts to simulate a multiphase interstellar medium on a kiloparsec scale in three dimensions with the stars and gas modeled self-consistently. Starting from inhomogenous initial conditions, our closed box simulations follow the gas as it cools and collapses under its own self-gravity to form stars which eventually return material and energy back through supernovae explosions and winds. This revised version was published online in August 2006 with corrections to the Cover Date.     

硅酸盐碳星的红外观测及能谱分布

本文对赤纬负10°以北的所有11颗硅酸盐碳星进行了近红外JHK观测．结合可见波段及红外天文卫星的观测结果,讨论了它们的红外双色图及能谱分布,并将其与正常碳星的结果相比较,进而讨论了它们的演化状态．     

顾及天线相位中心误差的SWARM卫星简化动力学精密定轨

对SWARM卫星进行简化动力学精密定轨，估计接收机天线相位中心偏差（PCO），并基于所得到的载波相位残差对天线相位中心变化（PCV）误差进行建模，验证其对轨道精度的影响。结果表明，当使用PCO信息时，定轨精度改善明显，径向、切向和法向的RMS值分别提升47%、48%和66%；加入PCV模型后，3个方向的精度有mm级的提升。SLR检核结果显示，同时考虑PCO和PCV，SWARM三颗卫星的平均RMS值为2.29 cm，与事后科学轨道十分接近。对比不同分辨率PCV模型定轨的结果发现，选择5°×5°PCV模型较为合适。     

白山拱坝位移激光监测自动化系统研究

提出用半导体激光发射器结合位敏传感器进行位移测量和利用光学测角仪进行倾角观测的方法解决拱坝变形观测问题。对激光监测自动化系统进行了原理分析、算法推导、精度评定。在白山拱坝的实践表明：本系统精度高，自动化效果好，具有较好的推广价值。     

拉曼后向散射在海面检测及海面与陆地区分中的应用

给出了光散射、后向散射以及拉曼后向散射等基本概念,推导了后向散射截面与后向散射微分截面的基本关系,以及散射微分截面的计算公式。同时还得出了振动拉曼散射、振动一转动拉曼散射、转动拉曼散射、瑞利散射之间的关系。提出了利用647nm红光的拉曼后向散射检测海面以及区分海面与陆地的方法,可以有效地提高机载激光海洋测深的精度。     

应用X射线源的航天器姿态测量

在介绍X射线源和X射线探测器、准直器的基础上,重点描述了应用X射线源测量航天器姿态参数的原理和方法。对X射线星扫描仪的结构、扫描观测X射线源方法和矩形准直器响应函数等做了介绍,较详细地论述了应用单准直器X射线星扫描仪和差分准直器X射线星扫描仪确定航天器姿态参数的测量模型,并进行了二者间的比较和分析。简单讨论了X射线星扫描仪测量建模和应用测量模型拟合航天器姿态参数的算法问题。最后,对采用编码孔径系统确定航天器姿态参数的方法做了概括性介绍。     

The effect of magnetic fields on star cluster formation

We examine the effect of magnetic fields on star cluster formation by performing simulations following the self-gravitating collapse of a turbulent molecular cloud to form stars in ideal magnetohydrodynamics. The collapse of the cloud is computed for global mass-to-flux ratios of  ∞, 20, 10, 5  and 3, i.e. using both weak and strong magnetic fields. Whilst even at very low strengths the magnetic field is able to significantly influence the star formation process, for magnetic fields with plasma  β < 1  the results are substantially different to the hydrodynamic case. In these cases we find large-scale magnetically supported voids imprinted in the cloud structure; anisotropic turbulent motions and column density striations aligned with the magnetic field lines, both of which have recently been observed in the Taurus molecular cloud. We also find strongly suppressed accretion in the magnetized runs, leading to up to a 75 per cent reduction in the amount of mass converted into stars over the course of the calculations and a more quiescent mode of star formation. There is also some indication that the relative formation efficiency of brown dwarfs is lower in the strongly magnetized runs due to a reduction in the importance of protostellar ejections.     

水下激光通讯发射接收系统

报导了可用于水下激光通讯的由８９ｃ５１单片机控制的全双工水下激光通讯系统实验装置。系统能有效的消除水下背景光的影响,并具有３～４个数量级动态范围的自动增益放大能力以更有效地接收水下激光通讯信号。能在水下以较高的数据传输率传递信息,数据传输率可以用软件调整,最大数据传输率为１９．２ｋＢｉｔｓ／ｓ。