V2213 Cyg is a New W Uma-Type System     

Elena Pavlenko  Anna Litvinchova 《Astrophysics and Space Science》2005,296(1-4):297-300

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.  相似文献   

A model of polarized OH maser emission in W75N     

M. D. Gray  B. Hutawarakorn  R. J. Cohen 《Monthly notices of the Royal Astronomical Society》2003,343(4):1067-1080

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

P. G. Niarchos 《Astrophysics and Space Science》2005,296(1-4):359-370

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.  相似文献   

Strong magnetic field in W75N OH maser flare     

V. I. Slysh  V. Migenes 《Monthly notices of the Royal Astronomical Society》2006,369(3):1497-1501

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.  相似文献   

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

G. N. Tsokas  G. C. Christofides  C. Papakonstantinou 《Pure and Applied Geophysics》1996,146(2):365-392

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.  相似文献   

赣南合龙钨矿矿床地质、成岩成矿时代与成矿模式     

尹政  赵正  陶建利  吴胜华  李宏伟  甘加伟  陈伟  李小伟 《岩石学报》2021,37(5):1531-1552

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。  相似文献   

Holocene record of productivity in the NW Iberian continental shelf     

V. Alves Martins  C. Patinha  E. Ferreira da Silva  J.-M. Jouanneau  O. Weber  F. Rocha   《Journal of Geochemical Exploration》2006,88(1-3):408

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.  相似文献   

A Technique for Direct Retrieval of Surface Specific Humidity Over Open Oceans from Irs-P4/Msmr Satellite Data     

Randhir Singh  B. Simon  P. C. Joshi 《Boundary-Layer Meteorology》2003,106(3):547-559

The Multi frequency Scanning Microwave Radiometer (MSMR) onboard Oceasat-1 was used to develop a retrieval method fornear-surface specific humidity by means of multivariate regressiontechnique. The MSMR measures the microwaveradiances in 8 channels at the frequencies of 6.6, 10.7, 18 and 21 GHzfor both vertical and horizontal polarizations. Regression coefficients were derived using the ship reports of the Comprehensive Ocean-Atmosphere Data Set (COADS) for the months of July, October and December, in 1999. Daily near-surface specific humidity data from COADS in 2° × 2° latitude/longitude bins and collocated brightness temperature data from MSMR were used to derive the coefficients. The derived coefficients werevalidated with humidity given in COADS.A linear relationship is established to determine the near-surface specifichumidity from MSMR brightness temperature (Tb) with an rms error of 1.2 g kg^-1 for individual situations and an rms errorof 0.84 g kg^-1 for monthly time scales over global oceans.The retrieval algorithm is validonly for the open sea regions.  相似文献   

The effect of water on accessory phase solubility in subaluminous and peralkaline granitic melts   总被引：4，自引：0，他引：4  

Robert L. Linnen   《Lithos》2005,80(1-4):267-280

The solubilities of columbite, tantalite, wolframite, rutile, zircon and hafnon were determined as a function of the water contents in peralkaline and subaluminous granite melts. All experiments were conducted at 1035 °C and 2 kbar and the water contents of the melts ranged from nominally dry to approximately 6 wt.% H₂O. Accessory phase solubilities are not affected by the water content of the peralkaline melt. By contrast, solubilities are affected by the water content of the subaluminous melt, where the solubilities of all the accessory phases examined increase with the water content of the melt, up to 2 wt.% H₂O. At higher water contents, solubilities are nearly constant. It can be concluded that water is not an important control of accessory phase solubility, although the water content will affect diffusivities of components in the melt, thus whether or not accessory phases will be present as restite material. The solubility behaviour in the subaluminous and peralkaline melts supports previous spectroscopic studies, which have observed differences in the coordination of high field strength elements in dry vs. wet subaluminous granitic glasses, but not for peralkaline granitic glasses. Lastly, the fact that wolframite solubility increases with increasing water content in the subaluminous melt suggests that tungsten dissolved as a hexavalent species.  相似文献   

垦利碱蓬Suaeda kenliensis J.W.Xing sp.nov.——碱蓬属一新种     

邢军武 《海洋科学》2018,42(9):51-54

报道了中国碱蓬属植物一新种——垦利碱蓬Suaeda kenliensis J.W.Xing sp.nov.。该种与南方碱蓬Suaeda australis(R.Br.)Moq.相近,但系一年生,种子具圆盘状和卵形两种形状,直径约2～3mm,叶长可达5～7 cm,无不定根,与南方碱蓬相区别。垦利碱蓬生长于潮间带和海水周期性淹没处。耐高盐,区域内海水盐度为25,滩涂表层含盐量在退潮后经日晒蒸发可达60‰以上。常形成单一种群的红海滩植被景观。模式标本存:中国科学院海洋生物标本馆;编号:MBM286537。采集地:莱州湾垦利海域潮间带泥滩。采集人:邢军武、曲宁、钟芳。  相似文献