The irregular galaxy Cassiopeia 1 – a new member of the Local group

A photometry in the V, R, I (Cousins) system has been performed for stars in the galaxy Cassiopeia 1. The resulting colour-agnitude (CM) diagram of Cas 1 reveals the existence of blue stars and the absence of red ones. From an analysis of the CM diagram of the galaxy it is concluded that A_v = 4.0 mag, and the distance modulus (m – M)_o = 24.5 mag, corresponding to a distance of 790 kpc. The visual magnitude of the galaxy is V = 14^m.62 (M_v = −13^m.8) and the colour index (V – R) = 0.89 mag. From the distance determination the galaxy Cassiopeia 1 is a member of the Local group.     

Java环境下基于Hibernate的GIS数据库访问策略

全关系型数据存储模式将GIS数据的空间数据和属性数据统一存储于关系数据库中,分析Java应用程序通过JDBC和SQL语言访问关系数据库中存储的GIS数据的不足,提出基于。Hibernate的解决方案,并给出地理信息共享系统的开发实例。     

中国西北侏罗纪煤系显微组分生烃潜力、产物地球化学特征及其意义

从吐哈盆地侏罗纪煤中分离富集了藻类体、孢子体、角质体、镜质体、基质镜质体和丝质体6种主要显微组分,进行了热解及热模拟实验,并对各显微组分热模拟生成的产物热解油进行了碳同位素组成等分析。各显微组分热解生烃潜力及其热解产物热解油的碳同位素组成表明,煤系有机质中藻类体的生油潜力最高,生成的液态烃类的碳同位素组成最轻;孢子体、角质体等陆源富氢组分生烃潜力低于藻类体,生成的液态烃类的碳同位素组成重于藻类体生成的液态烃类,与煤系含油气盆地中原油的碳同位素组成基本一致。这些富氢显微组分应该是煤系有机质中主要的生油显微组分。镜质体和基质镜质体的生油潜力相对较低,其生成的液态烃类的碳同位素组成比一般煤系原油重得多,而且这些组分本身对液态烃具有较强的吸附力,尽管其在煤系有机质中所占的比例很大,仍然难以成为生成液态石油的主要显微组分,只能在高成熟演化阶段成为良好的生气显微组分。丝质体等惰性组分生烃潜力极低,不可能成为生油组分。此外,结合原煤的显微组分组成、生烃潜力和元素分析,提出仅仅以壳质组的含量高低来评价煤的生烃潜力不完全可靠,热解是经济、快速、有效的评价方法。     

龙骨坡遗址第7水平层石制品新材料

文章记述并分析了20世纪90年代后期重庆巫山龙骨坡遗址出土于第7水平层的16件石制品,包括若干各具特色的工具类型,如原型手镐、原型薄刃斧、大型尖刃器、直刃砍砸器、凸刃砍砸器、长刃石刀、短刃石刀、刮削器、凿刃器等,反映出石器制作者明确的工作目标和为了达到目标所经历的一个又一个中间过程;说明了当时的人类对工具制作的具体需求和适当利用自然环境的事实。研究证据还体现了大约200万年前华南早期人类工具类型的多样性与特殊性,标志着中国早期人类在当时阶段所达到的技术发展水平。龙骨坡遗址很可能是东亚早期人类文化的一个发祥地。     

基于小波变换的射频干扰消除方法的研究

在射电天文观测中,射频干扰(Radio Frequency Interference, RFI)会以多种形式混入望远镜接收系统,给观测带来误判或者降低观测信噪比.近年来国内国际射电天文快速发展,国内国际大型射电望远镜和阵列先后建设,观测灵敏度大为提高,射频干扰的影响尤为突出.随着科技发展和人类活动的加剧,射频干扰日益严重且不可逆转.提出利用2维离散小波变换的方法分析射电天文观测的数据,对望远镜系统输出的时间频率序列进行小波变换,根据小波系数分离出原始信号中各分量,每个分量统计得到相应的阈值,将各分量与阈值相比较识别干扰成分并标记去除.利用该方法对实际观测数据进行了处理,结果表明该方法能够很好地标记并消减干扰信号,且提高了观测的信噪比.     

The Basic Shape Classification of Space Debris with Light Curves

We study the machine learning method for classifying the basic shape of space debris in both simulated and observed data experiments, where light curves are used as the input features. In the dataset for training and testing, simulated light curves are derived from four types of debris within different shapes and materials. Observed light curves are extracted from Mini-Mega TORTORA (MMT) database which is a publicly accessible source of space object photometric records. The experiments employ the deep convolutional neural network, make comparisons with other machine learning algorithms, and the results show CNN (Convolutional Neural Network) is better. In simulational experiments, both types of cylinder can be distinguished perfectly, and two other types of satellite have around 90% probability to be classified. Rockets and defunct satellites can achieve 99% success rate in binary classification, but in further sub-classes classifications, the rate becomes relatively lower.     

焦作市矿产资源开发的环境地质问题

焦作市是在矿产资源开发基础上建立起来的新兴工业城市,随着社会经济的发展,环境地质问题日益突出。现有采空区149 km2,煤矸石堆存量1 180.77×104t,占地41.81×104m2,尾矿坝4座,方量已达2 660×104m3,矿坑突水700余次,经济损失达3亿多元,矿区水环境污染严重,大部分地下水为Ⅳ类、Ⅴ类水。每年投入治理与赔偿地面变形、塌陷损失金额达数百万元。本文分析认为矿产资源开发环境保护的法律法规不健全,环境保护意识淡薄,矿区环境恢复治理资金不畅,技术投入不足是造成矿区生态环境地质问题与影响矿区生态环境治理的主要因素。加强宣传教育,推广实用技术,从源头减少矿产资源开发诱发的环境地质问题,建立矿山生态环境保护与恢复治理相关制度,实施矿业权资产化管理,是有效预防因矿产资源开发诱发生态环境恶化及进行恢复治理的重要途径。     

The additional radiation of Cyg X-1 at primary minimum

New UBV-photoelectric observations of the well-known massive X-ray binary system Cyg X-1/V 1357 Cyg are obtained near the primary minimum. The detailed analysis of these observations confirms the existence of additional blue radiation which appears as a narrow peak with an amplitude of 0.01–0.02 mag near phase 0.00 on the light curve (the superior conjunction of the relativistic component), firstly detected by Lyuty (1985). This emission does not appear at every orbital cycle. The appearance of this narrow peak of additional blue radiation on the light curve of Cyg X-1 can be explained as the radiation of relativistic electrons in the disturbed magnetic field of the optical star in frames of the model proposed by Ikhsanov and Fabrika (1990).     

Stream formation in W Serpentis-type binaries

By the method proposed by Nazarenko (1993) and using observational data obtained by different authors, the physical conditions in the stream in the neighbourhood of the inner Lagrangian point L₁ were calculated for three interacting binary systems of W Ser-type: β Lyr, V367 Cyg, RY Sct. It is shown, that as a result of the evolutional expansion of the mass losing component the deep layers of its atmosphere reach the neighbourhood of the first Lagrangian point L₁ and a stream of axial symmetric shape is formed. Its radius is comparable to the dimension of the mass losing component. The rate of the mass transfer increases up to 10⁻⁵ M_⊙/yr. The calculated parameters of the stream in the neighbourhood of the point L₁ explain the main observational properties of the investigated systems (existence of extended circumstellar matter with a developed structure, high mass transfer rate).     

The problem of the sighting line stabilization for axial meridian circles

The paper deals with the method based on treating the axial meridian circle and a long-focus light mark in the prime vertical as a single virtual instrument that has properties of meridian circle. A horizontal axis, a sighting line, and a micrometer cross-wire of the instrument are created by optical means. The key function here is performed by the light mark that ensures a reference direction used for formation of instrumental principal planes and directions. Stability of instrumental azimuth, inclination, and collimation is expected to be about ±0.″01. Besides, an accuracy of observations is not affected by any temperature and weight deformations of telescope mechanics. Owing to the last circumstance, the design is cheap and the telescope aperture may be increased significantly, to about 1m. An estimate of accuracy of observations depends on the adopted model of image motion, and for sites with excellent seeing and bright stars is ±0.″03 to ±0.″05 (rms).