V2213 Cyg is a New W Uma-Type System

V2213 Cyg was discovered as a variable star by Pavlenko (1999) in 1998. We present our photometry of V2213 Cyg from 1998–2003 based on CCD observations with the K-380 Cassegrain telescope of CrAO and the 60 cm Zeiss telescope of SAI. Observations have been carried out mostly in R and sometimes in B and V Johnson system. The total amount of data is 2270 points, covering ∼50 nights. We classify this binary as a W UMa-type contact system. Using all data we determined the orbital period to be 0.350079 ± 0.000007 day. The mean brightness varies between R = 14.35 and 14.05. The mean 1999–2003 orbital light curve has two humps and a primary minimum (I), which is 0.04 mag brighter than the deeper secondary one (II). The mean humps have slightly different height. The difference between two individual maxima varies within 0.1 mag, which may indicate an activity of the components. The highest hump is an asymmetrical one: it has sort of a shoulder at phases 0.75–0.80, before entering the less deep primary minimum (phase 0.0). The system is rather reddened, its colour indices are: B−V ∼ 0.8 and V−R ∼ 0.7, and give a spectral class of V2213 Cyg earlier than K.     

Contact Binaries: A Study of the Proximity Effects and Gravity Darkening Based on Kopal’s Fourier Method

A new method for the determination of the proximity effects and gravity darkening exponents in contact binaries of W UMa type is presented. The method is based on Kopal’s method of Fourier analysis of the light changes of eclipsing variables in the Frequency Domain. The method was applied to 36 W UMa systems for which geometric and photometric elements have been derived by the most powerful techniques. The derived values are very close to those predicted by the existing theory of radiative transfer or convective equilibrium.     

Strong magnetic field in W75N OH maser flare

A flare of OH maser emission was discovered in W75N in 2000. Its location was determined with the Very Long Baseline Array (VLBA) to be within 110 au from one of the ultracompact H  ii regions, Very Large Array 2 (VLA2). The flare consisted of several maser spots. Four of the spots were found to form Zeeman pairs, all of them with a magnetic field strength of about 40 mG. This is the highest ever magnetic field strength found in OH masers, an order of magnitude higher than in typical OH masers. Three possible sources for the enhanced magnetic field are discussed: (i) the magnetic field of the exciting star dragged out by the stellar wind; (ii) the general interstellar field in the gas compressed by the magnetohydrodynamic shock; and (iii) the magnetic field of planets which orbit the exciting star and produce maser emission in gaseous envelopes.     

藏北南羌塘盆地曲瑞恰乃地区中侏罗世色哇组、莎巧木组、布曲组的生物地层特征

对藏北南羌塘盆地曲瑞恰乃地区的晚三叠世-侏罗纪地层进行了研究,自下而上划分为晚三叠世日干配错群,晚三叠世～早侏罗世索布查组,早侏罗世曲色组,中侏罗世色哇组、莎巧木组、布曲组、夏里组和晚侏罗世索瓦组。其中,对中侏罗世色哇组、莎巧木组、布曲组生物地层的研究为本文的主要内容,研究成果为该区中侏罗世地层层序的建立和详细对比提供了重要的依据。     

A geophysical study of the granites and the sedimentary basins of the Xanthi area (N. Greece)

Intrusive features of varying size can be interpreted from the aeromagnetic map of the Xanthi area in N. Greece.The Xanthi pluton, which outcrops north of the city of Xanthi, seems to have the shape of a truncated pyramid. This feature has relatively large areal extent and reaches an approximate depth of 7 km. Another, relatively large magnetic body is buried under the sediments at the estuary of the Nestos River.3-D models of several smaller intrusions were constructed and the produced effect was compared to the observed. Some of these intrusions seem to be detached branches of the large Xanthi pluton.The basement in the outer part of the basin of the Nestos River seems to be buried at about 4 km depth. This figure is obtained by the Multiple Source Werner Deconvolution estimates and it is in agreement with the results of former geophysical studies and deep industrial boreholes.A 3-D model of the Xanthi-Komotini basin suggests that this basin is about 0.4 km deep at its southern part. The depth at its northern boundary is about 1.8 km while the boundary itself is formed by the large Kavala-Xanthi-Komotini fault.The Tertiary basin of the Nestos River and the observed magmatism are consistent with the idea of an older extensional tectonic regime in the area.     

相律的应用:蒸发结晶过程自由度

在连续原理和浓度限制条件的基础上,分析了卤水蒸发过程的自由度,提出了“蒸发结晶过程自由度”这一概念。发现蒸发结晶过程自由度在整个过程中不是1便是0,在1和0之间交替变化,与选择的组分数和析出固相数目无关。蒸发结晶过程自由度为1,物理意义是在不引起新相产生旧相不消失的前提下过程连续地变化(水分的连续蒸失),几何意义是指在适当的坐标系中的一条线,一条直线或曲线;0的物理意义是指新相的产生和旧相的即将消失或者前一段的连续变化过渡到后一段的连续变化,几何意义是指一点,两蒸发阶段的交点或者过程的终点。简单地讨论了过程的单向性和连续件。     

赣南合龙钨矿矿床地质、成岩成矿时代与成矿模式

合龙钨矿床位于南岭东西向构造岩浆带与北-北东向于山构造带交汇部位,是南岭东段于都-赣县矿集区的重要组成。合龙钨矿床是赣南地区近年在石英脉型钨矿勘查取得最重要突破的矿区,新发现钨多金属矿体达48条,新探明黑钨矿资源量3.5万余吨,WO_3平均品位2.189%,深部具有大型以上资源潜力。合龙钨矿床以外带石英大脉型矿体与岩体内石英细脉-云英岩型钨矿体分带共生为特色,区别于经典的石英脉型钨矿床的"五层楼"分带,也不同于"西华山式"仅岩体内成矿和"盘古山式"的仅岩体外成矿,故对其开展成岩成矿时差研究、内外带成矿过程对比研究和成矿模式研究具有重要意义。本文在矿床地质工作基础之上,对该矿床进行了较详细的矿物学研究,对比了不同阶段、不同分带黑钨矿和白钨矿的矿物化学特征;应用LA-ICP-MS锆石U-Pb法获得深部隐伏中细粒斑状黑云母花岗岩的成岩年龄为159.0Ma;应用辉钼矿Re-Os等时线法,测定了内带石英脉-云英岩型矿体成矿时代为157.3Ma,外带石英脉型矿体成矿时代为159.6Ma。研究表明,合龙钨矿床形成于燕山早期,是华南东部中生代大规模花岗质岩浆活动与钨多金属成矿作用的产物,其成矿作用紧随花岗质岩浆侵入而发生,成岩与成矿时间基本一致。内脉带矿化略晚于外脉带钨矿化,外脉带黑钨矿以相对高温阶段形成的含锰钨铁矿为主,内脉带黑钨矿则以成矿作用中晚期的含铁钨锰矿为主。基于上述研究成果,本文建立了"合龙式"钨矿床成矿模式,对石英脉-云英岩型钨矿成矿理论研究具有一定的推动作用,对下一步勘查工作部署具有重要实践意义。     

Holocene record of productivity in the NW Iberian continental shelf

A multiproxy approach (textural characteristics, heavy metal concentrations and benthic foraminifera data) was adopted to study the OMEX core KSGX 40, collected at the Galicia Mud Deposit (NW Iberian outer continental shelf) and recording the last ca. 4.8 ka cal BP. Geochemical profiles of Fe, Mn, Zn, Co, Cr, Cu, Ni, Pb, Al and Ca show significant temporal variations. Benthic foraminifera productivity proxy suggests that the recorded muddy events were contemporaneous of a higher C_org flux to the marine benthic environment. The higher flux of organic matter, following a long-term intensification of the upwelling and coinciding with a finer sedimentation, led to depressed levels of oxygen beneath the water-sediments interface and to early diagenetic processes of several redox-sensitive elements.     

可可西里——东昆仑活动构造带强震活动研究

青海昆仑山口西 8.1级地震发生在具有新生性特征的可可西里—东昆仑活动断裂带上。该断裂带在 190 0年以来的 10 0多年中经历了一个强震活动过程。在该强震活动过程中 ,地震沿整个可可西里—东昆仑活动构造带分段破裂 ,强震的破裂长度和震级之间大致满足对数线性的统计关系 ,强震活动呈现指数型时间分布的加速特征。这种强震加速活动特征可以用含多个震源体的孕震系统的强震成组活动模型给予解释。