基于区域监测站的BDS定轨策略分析

围绕影响轨道精度和实时性的5个要素（模糊度分类固定、测站数量、定轨弧长、太阳光压模型和多系统组合）展开研究,得出区域测站分布下的定轨优选策略。实验表明,选取中国区域27个均匀分布的地面区域监测站,利用72 h弧长观测数据,采用ECOM 5参数简化太阳光压摄动模型、BDS/GPS双系统联合定轨可达到较好的精度,其中GEO卫星轨道精度约291 cm,IGSO/MEO卫星轨道精度优于11 cm。若BDS单系统采用上述策略进行定轨,也可达到GEO卫星299 cm和IGSO/MEO卫星14.4 cm的近似等价定轨精度。     

世越号起吊姿态敏感性分析与方案选择

韩国世越号打捞是世界上首次利用托底钢梁原状态整体起吊难船出水的工程。客滚难船装载的货物容易在沉没后发生移位,上层建筑长时间沉没海底后发生泥沙淤积导致难以准确估计整船的重量重心及浮力浮心的位置。利用水池模型试验和数值计算两种方法分别对大型浮吊船单臂架打捞法和双驳船抬吊打捞法进行了难船姿态受重心位置偏移的敏感性分析。水池模型试验中发现,用大型浮吊船单臂架打捞法,世越号的姿态受其重心位置偏移非常敏感,容易发生侧翻;而用双驳船抬吊打捞法,世越号的姿态受其重心位置的影响非常有限,难船和抬浮驳船都可以保持一个较好的姿态。对比水池模型试验的结果,由于难以计及托底钢梁的翘动和滑动现象,数值计算中得到的难船起吊姿态值偏小。双驳船抬吊打捞法被选为打捞世越号的施工方案,其对难船重心位置偏移不敏感的特性得到了现场实证。这个特点为世越号的成功打捞出水起到了关键作用。     

Magnetic Disconnections at the Boundary of a Small Interplanetary Magnetic Flux Rope Associated with a Reconnection Exhaust

A local current sheet and a subsequent small interplanetary magnetic-flux rope were observed on 1 April 2003 by Wind and the Advanced Composition Explorer (ACE). A Petschek reconnection-like exhaust crossing of the local current sheet was identified using the Walén test. The Wind spacecraft re-entered the reconnection exhaust after the main exhaust encounter, and the reentry may be due to a spatial fold of the current-sheet surface itself. The absence of parallel strahls and the presence of antiparallel strahls on either side of the current sheet suggest that the magnetic-field lines before the exhaust and in the subsequent small flux rope are all open. The \(180^{\circ}\) pitch-angle strahls were clearly absent, and halo-suprathermal electron pitch-angle distributions were observed in the exhaust. This finding means that the open field lines of the magnetic-flux rope were reconnecting to the adjacent open field lines to produce U-shaped field lines disconnected from the Sun. These observations provide direct evidence that the magnetic fields of the interplanetary small magnetic-flux rope were disconnecting from the Sun through magnetic reconnection. This type of disconnected event potentially has important implications for the magnetic-flux budget of the heliosphere.     

Antenna design and implementation for the future space Ultra-Long wavelength radio telescope

In radio astronomy, the Ultra-Long Wavelengths (ULW) regime of longer than 10 m (frequencies below 30 MHz), remains the last virtually unexplored window of the celestial electromagnetic spectrum. The strength of the science case for extending radio astronomy into the ULW window is growing. However, the opaqueness of the Earth’s ionosphere makes ULW observations by ground-based facilities practically impossible. Furthermore, the ULW spectrum is full of anthropogenic radio frequency interference (RFI). The only radical solution for both problems is in placing an ULW astronomy facility in space. We present a concept of a key element of a space-borne ULW array facility, an antenna that addresses radio astronomical specifications. A tripole–type antenna and amplifier are analysed as a solution for ULW implementation. A receiver system with a low power dissipation is discussed as well. The active antenna is optimized to operate at the noise level defined by the celestial emission in the frequency band 1 ? 30 MHz. Field experiments with a prototype tripole antenna enabled estimates of the system noise temperature. They indicated that the proposed concept meets the requirements of a space-borne ULW array facility.     

SONG-China Project: A Global Automated Observation Networktwo

Driven by the technological advancements and scientific objectives, the data acquisition in observational astronomy has been changed greatly in recent years. Fully automated or even autonomous ground-based network of telescopes has now become a tendency for time-domain observational projects. The Stellar Observations Network Group (SONG) is an international collaboration with the participation and contribution of the Chinese astronomy community. The scientific goal of SONG is time-domain astrophysics, such as the astroseismology and the research of variable stars in open clusters. The SONG project aims to build a global network of one-meter telescopes equipped with high-precision and high-resolution spectrographs, and two-channel lucky-imaging cameras. It is the Chinese initiative to install a 50 cm binocular photometry telescope at each SONG node to share the network platform and infrastructure. This work is focused on the design and implementation of SONG/50BiN in technology and methodology, for the ground-based network composed of multiple sites and a variety of instruments.     

Radio variability of the blazar S5 0716+714: a ∼6.1 year quasi-periodicity

We report a ～6.1 yr quasi-periodicity for the blazar S5 0716+714 using the radio light curves at 4.8, 8 and 14.5 GHz observed by the University of Michigan Radio Astronomical Observatory (UMRAO) from 1981 to 2012, by means of the Jurkevich, discrete correlation function (DCF) and power spectral analysis techniques. There are a general correlation among light curves at different frequencies and a time lag of \(170\pm 10\) days between 4.8 and 14.5 GHz light curves can be confirmed. We also estimate the orbit parameters assuming a binary black hole system, and the magnetic field strength under the jet comoving frame.     

黄河流域地下水资源、主要环境地质问题及对策建议

本文在重新汇总黄河流域地下水资源量的基础上 ,提供黄河流域天然补给资源总量为453 .54亿m3 /a,其中淡水为 40 3 .51亿m3 /a,微咸水补给约 50 .0 3亿m3 /a。可开采资源总量为2 1 2 .2 4亿m3 /a,其中淡水为 1 82 .42亿m3 /a,微咸水约 2 9.82亿m3 /a。总结分析了黄河流域主要环境地质问题的发展趋势 ,提出了水资源利用方面的一系列宏观对策建议。     

从成矿和变形时代的不耦合现象探讨康古尔金矿的成因

位于塔里木盆地北缘的康古尔金矿出露于秋格明塔什-黄山巨型韧性剪切带中部，长期以来被当作剪切带型金矿加以研究。通过初步的同位素年代学研究却发现了成矿和变形时代的不耦合现象：康古尔金矿成矿时代在290Ma左右，而秋格明塔什-黄山韧性翦切带剪切变形时代在225～236Ma。如果认定康古尔金矿成矿作用发生在海西期，则发生于印支中-晚期的韧性剪切变形作用不仅不是康古尔金矿成矿作用的主因，而且对金矿的改造作用也是有限的。因此，康古尔金矿不能被称为剪切带型金矿。     

用于同位素测年的自生伊利石分离纯化流程探索

沉积岩中自生矿物与碎屑矿物的分离问题是制约沉积岩定年的主要问题之一。本文以浙江和川西地区的粘土矿物为例，介绍了沉积岩中自生伊利石与碎屑矿物的一般分离过程，具体包括悬浮液的制备过程、高速离心机的条件实验和8个样品的分级实验，确定了较佳的分级参数，并对分级后的各级别进行了X-射线衍射(XRD)分析。X-射线衍射结果表明，随着粒度的减小，各种杂质的含量都在逐渐减少，在小于0．2μm的粒级中，已检测不出石英、钾长石、钠长石、方解石、白云石等杂质的存在，其中有3个产品的成岩混层含量达到100％，说明本次实验的分离纯化流程是比较成功的。综合考虑粒度和自生伊利石的纯度，一般情况下，以0．1～0．2μg粒级的产品用于Ar-Ar和K-Ar测年较合适。但在实际进行年龄分析时，一定要先进行XRD和透射电镜分析，只有确定其成岩混层I／S的含量近100％(至少在95％以上)及混层中S的含量小于25％时，才可用于Ar—Ar和K—Ar年龄测定。