胶东半岛乳山地区低角度韧性剪切带几何学、运动学特征:对中国东部岩石圈减薄作用的启示

大规模伸展构造是华北克拉通东部岩石圈减薄的重要表现形式。部分低角度韧性剪切带是地壳伸展变形后所展现的构造形式。本文研究了王格庄韧性剪切带的岩石学、几何学、运动学等特征显示:韧性剪切带走向近南北向,剪切带断层面倾向多变(倾向西、西南、西北方向)。大部分区域面理低角度倾向西,矿物拉伸线理近东西向,不对称旋转碎斑及S-C组构指示顶端指向西的剪切特征。结合研究区西侧与伸展构造相匹配的半地堑伸展盆地证据:本研究认为伸展构造的形成可能与西太平洋板块的后撤相关,即大规模伸展构造作用引发了华北克拉通东部的地壳减薄作用。     

基于遥感的上海地区雾霾监测研究

以中分辨率成像光谱仪(MODIS)遥感数据为数据源,综合利用6S传输模型与NASA V5.2算法对2013年12月4日至8日上海地区雾霾污染进行了连续性监测,并对其形成原因进行分析。结果表明,此次雾霾污染主要是由本地生产和外地迁移来源共同作用形成,上海地区气溶胶光学厚度在12月6日达到最大,雾霾污染区域逐渐从上海地区的西北向东南扩散,污染等级也逐渐降低。     

海岸线及其测绘技术探讨

海岸线是人类所使用的最古老的边界线之一,然而,由于其动态特征,加之当今社会对海岸带的需求越来越多,这条边界线的位置存在争议,因而,如何使用客观手段测绘海岸线尤为重要。文中针对海岸线定义及其位置确定不明确的现状,指出海岸线定义存在的问题,给出完善定义的意见;分析海岸线常规的测绘方法,探讨海岸线精确测绘的新方法和技术。     

陕北奥陶纪盐盆马五6时期东、西部盐坳沉积环境对比研究

陕北奥陶纪盐盆位于鄂尔多斯盆地伊陕斜坡东部。研究表明:马五6亚期,盐盆存在"两坳一隆"的构造格局,即东、西部盐坳和中部隆起,东、西部盐坳在钾矿化情况、溴氯系数反映的水体咸化趋势方面初步显示了陕北盐盆东、西部沉积环境的差异。本文通过东、西部盐坳典型钻井马五6层位沉积学分析,揭示了马五6时期东、西部盐坳在水体深度变化、浓缩趋势、含钾量、淡化层段厚度、陆源物质输入方面均存在差异。其中,西部盐坳受海水影响大,水体变浅且持续淡化,泥质分布反映陆源物质贡献少,对钾盐的沉积与保存均十分不利。而东部盐坳受海水影响小,与西部盐坳水体联通性差,在马五6时期环境更为封闭,具体表现为淡化夹层分布数量少、厚度薄的特征;水体持续变深并浓缩咸化;泥质夹层较多,反映了相较于西部,陆源物质对其影响更大,上述特点为钾盐沉积提供了有利的地球化学条件及可容空间。东、西部盐坳沉积环境对比表明东部盐坳对成钾更为有利。     

Masses of the local group and of the M81 group estimated from distortions in the local velocity field

Based on high precision measurements of the distances to nearby galaxies with the Hubble telescope, we have determined the radii of the zero velocity spheres for the local group, R₀ = 0.96±0.03Mpc, and for the group of galaxies around M 81/M 82, 0.89±0.05Mpc. These yield estimates of M_T = (1.29±0.14)· 10¹² M_⊙ and (1.03±0.17)· 10¹² M_⊙, respectively, for the total masses of these groups. The R₀ method allows us to determine the mass ratios for the two brightest members in both groups, as well. By varying the position of the center of mass between the two principal members of a group to obtain minimal scatter in the galaxies on a Hubble diagram, we find mass ratios of 0.8:1.0 for our galaxy and Andromeda and 0.54:1.00 for the M82 and M81 galaxies, in good agreement with the observed ratios of the luminosities of these galaxies. __________ Translated from Astrofizika, Vol. 49, No. 1, pp. 5–22 (February 2006).     

Unravelling the mystery of the M31 bar

The inclination of M31 is too close to edge-on for a bar component to be easily recognized and is not sufficiently edge-on for a boxy/peanut bulge to protrude clearly out of the equatorial plane. Nevertheless, a sufficient number of clues allow us to argue that this galaxy is barred. We use fully self-consistent N -body simulations of barred galaxies and compare them with both photometric and kinematic observational data for M31. In particular, we rely on the near-infrared photometry presented in a companion paper. We compare isodensity contours to isophotal contours and the light profile along cuts parallel to the galaxy major axis and offset towards the north, or the south, to mass profiles along similar cuts on the model. All these comparisons, as well as position–velocity diagrams for the gaseous component, give us strong arguments that M31 is barred. We compare four fiducial N -body models to the data and thus set constraints on the parameters of the M31 bar, as its strength, length and orientation. Our 'best' models, although not meant to be exact models of M31, reproduce in a very satisfactory way the main relevant observations. We present arguments that M31 has both a classical and a boxy/peanut bulge. Its pseudo-ring-like structure at roughly 50 arcmin is near the outer Lindblad resonance of the bar and could thus be an outer ring, as often observed in barred galaxies. The shape of the isophotes also argues that the vertically thin part of the M31 bar extends considerably further out than its boxy bulge, that is, that the boxy bulge is only part of the bar, thus confirming predictions from orbital structure studies and from previous N -body simulations. It seems very likely that the backbone of M31's boxy bulge is families of periodic orbits, members of the x₁-tree and bifurcating from the x₁ family at its higher order vertical resonances, such as the x1v3 or x1v4 families.     

A new red variable star in the globularcluster M4

G302 = L3107 is a red star located at the lowest end of the red giant branch of the globular cluster M4. According to its location on the C-M diagram, G302 may be a cluster member. No proper motion or radial velocity determinations are available up to date.

We discovered that C302 is a new variable star with a main period of 1.24719 day and a peak to peak amplitude of about 0.3 mag in V. It may have a second period of 2.38249 day with an amplitude of about 0.05 mag. If it is a cluster member, then there will be interesting implications for the the theory of stellar evolution.     

Searching for Variable Stars in and around Open Clusters

We present a snapshot of our recent results of a variable star survey in 1 degree fields around three open clusters: NGC 188, NGC 7789 and M67. A total number of 39 variable stars are newly discovered, including 22 W UMa stars, 10 EA (Algol) type binaries, one RR-lyr and one RRd pulsator, and five unclassified variables.