First detection of a magnetic field in the fast rotating runaway Oe star ζ Ophiuchi     

S. Hubrig  L.M. Oskinova  M. Schller 《Astronomische Nachrichten》2011,332(2):147-152

The star ζ Ophiuchi is one of the brightest massive stars in the northern hemisphere and was intensively studied in various wavelength domains. The currently available observational material suggests that certain observed phenomena are related to the presence of a magnetic field. We acquired spectropolarimetric observations of ζ Oph with FORS 1 mounted on the 8‐m Kueyen telescope of the VLT to investigate if a magnetic field is indeed present in this star. Using all available absorption lines, we detect a mean longitudinal magnetic field 〈B_z〉_all = 141 ± 45 G, confirming the magnetic nature of this star. We review the X‐ray properties of ζ Oph with the aim to understand whether the X‐ray emission of ζ Oph is dominated by magnetic or by wind instability processes (© 2011 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

利用Excel VBA自动绘制物化探平剖图   总被引：3，自引：0，他引：3  

王芳  李波  刘慧鹏 《云南地质》2010,29(2):231-234

提出在Excel VBA平台,结合Active X技术,自动实现平剖面图的数据整理及Surfer成图,应用于云南中甸铅锌矿数据成图工作,取得满意效果。  相似文献   

Amphibolites with staurolite and other aluminous minerals: calculated mineral equilibria in NCFMASH   总被引：1，自引：0，他引：1  

Arnold  Powell  & Sandiford 《Journal of Metamorphic Geology》2000,18(1):23-40

Amphibolite facies mafic rocks that consist mainly of hornblende, plagioclase and quartz may also contain combinations of chlorite, garnet, epidote, and, more unusually, staurolite, kyanite, sillimanite, cordierite and orthoamphiboles. Such assemblages can provide tighter constraints on the pressure and temperature evolution of metamorphic terranes than is usually possible from metabasites. Because of the high variance of most of the assemblages, the phase relationships in amphibolites depend on rock composition, in addition to pressure, temperature and fluid composition. The mineral equilibria in the Na₂O–CaO–FeO–MgO–Al₂O₃–SiO₂–H₂O (NCFMASH) model system demonstrate that aluminium content is critical in controlling the occurrence of assemblages involving hornblende with aluminous minerals such as sillimanite, kyanite, staurolite and cordierite. Except in aluminous compositions, these assemblages are restricted to higher pressures. The iron to magnesium ratio (X_Fe), and to a lesser extent, sodium to calcium ratio, have important roles in determining which (if any) of the aluminous minerals occur under particular pressure–temperature conditions. Where aluminous minerals occur in amphibolites, the P–T–X dependence of their phase relationships is remarkably similar to that in metapelitic rocks. The mineral assemblages of Fe‐rich amphibolites are typically dominated by garnet‐ and staurolite‐bearing assemblages, whereas their more Mg‐rich counterparts contain chlorite and cordierite. Assemblages involving staurolite–hornblende can occur over a wide range of pressures (4–10 kbar) at temperatures of 560–650 °C; however, except in the more aluminous, iron‐rich compositions, they occupy a narrow pressure–temperature window. Thus, although their occurrence in ‘typical’ amphibolites may be indicative of relatively high pressure metamorphism, in more aluminous compositions their interpretation is less straightforward.  相似文献   

The applications of the MHD Alfvén wave oscillation model for kHz quasi‐periodic oscillations     

C.M. Zhang  H.X. Yin  Y.H. Zhao  H.K. Chang  L.M. Song 《Astronomische Nachrichten》2007,328(6):491-498

In this paper, we improve the previous work on the MHD Alfvén wave oscillation model for the neutron star (NS) kHz quasi‐periodic oscillations (QPOs), and compare the model with the updated twin kHz QPO data. For the 17 NS X‐ray sources with the simultaneously detected twin kHz QPO frequencies, the stellar mass M and radius R constraints are given by means of the derived parameter A in the model, which is associated with the averaged mass density of the star as 〈ρ 〉 = 3M /(4πR³) ≃ 2.4 × 10¹⁴ (A /0.7)² g/cm³, and we also compare the M ‐R constraints with the stellar equations of state. Moreover, we also discuss the theoretical maximum kHz QPO frequency and maximum twin peak separation, and some expectations on SAX J1808.4–3658 are mentioned, such as its highest kHz QPO frequency ∼ 870 Hz, which is about 1.4–1.5 times less than those of the other known kHz QPO sources. The estimated magnetic fields for both Z sources (about Eddington accretion rate ) and Atoll sources (∼ 1% ) are approximately ∼10⁹ G and ∼10⁸ G, respectively. (© 2007 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

A near‐infrared/optical/X‐ray survey in the centre of σ Orionis     

J.A. Caballero 《Astronomische Nachrichten》2007,328(9):917-927

Because of the intense brightness of the OB‐type multiple star system σ Ori, the low‐mass stellar and substellar populations close to the centre of the very young σ Orionis cluster is poorly know. I present an IJHK_s survey in the cluster centre, able to detect from the massive early‐type stars down to cluster members below the deuterium burning mass limit. The near‐infrared and optical data have been complemented with X‐ray imaging. Ten objects have been found for the first time to display high‐energy emission. Previously known stars with clear spectroscopic youth indicators and/or X‐ray emission define a clear sequence in the I vs. I – K_s diagram. I have found six new candidate cluster members that follow this sequence. One of them, in the magnitude interval of the brown dwarfs in the cluster, displays X‐ray emission and a very red J – K_s colour, indicative of a disc. Other three low‐mass stars have excesses in the K_s band as well. The frequency of X‐ray emitters in the area is 80±20 %. The spatial density of stars is very high, of up to 1.6±0.1 arcmin^–2. There is no indication of lower abundance of substellar objects in the cluster centre. Finally, I also report two cluster stars with X‐ray emission located at only 8000–11000 AU to σ Ori AB, two sources with peculiar colours and an object with X‐ray emission and near‐infrared magnitudes similar to those of previously‐known substellar objects in the cluster. (© 2007 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

珊瑚的影像密度恢复南海海表温度   总被引：7，自引：0，他引：7  

何学贤  彭子成  王兆荣  聂宝符  陈特固  王路 《地理学报》2000,55(2):183-190

将南海西沙永兴岛 ( 1 6°50′N,1 1 2°2 0′E)西北的造礁珊瑚的岩芯 ,制成 X射线负片。用显微光密度计在 X射线负片上获得沿生长轴方向的影像密度值 ,时间序列为 1 937～ 1 993年。根据影像密度数据 ,计算出珊瑚的各年生长率和钙化率的代用指标。珊瑚生长率和钙化率的代用指标都与 SST呈显著正相关。根据 1 960～ 1 993年的资料统计 ,相关系数分别是 0 .91和 0 .85,从而建立了珊瑚生长率温度计和钙化率代用指标温度计。并用这两个温度计测算到 1 937年 ,揭示出南海的 SST变化既受到全球气候环境变化为主的影响 ,也受到半封闭海域格局的影响  相似文献   

含Mg矿物和玻璃中Mg的局部结构研究   总被引：2，自引：1，他引：1  

彭明生  李迪恩 《矿物学报》2000,20(3):220-223

本文用同步辐射的MgK-边X射线近边结构谱(XANES)研究了9种含Mg矿物的MgK-边特征谱,其谱的能量位置随着配位数的增加而增大;建立了含Mg矿物中Mgk-边的能量与Mg-O键距的关系CaMgSi2O6(Di)-NaAlSi3O8(Ab)玻璃中MgK-边XANES的能量和Mg-O的键长的关系.在Di-Ab玻璃中的Mg-O键距是0.2±0.004nm.表明本方法可以作为研究含Mg矿物Mg的配位与局部结构新的结构探针.  相似文献   

叠前地震资料噪声衰减的小波域方法研究   总被引：45，自引：5，他引：40       下载免费PDF全文

高静怀  毛剑  满蔚仕  陈文超  郑庆庆 《地球物理学报》2006,49(4):1155-1163

讨论了叠前地震记录中随机噪声的模拟方法,采用定性分析与Monte Carlo仿真相结合的方法,研究了在物理小波为基本小波的变换域该类随机噪声局部小波功率谱的统计特性,得出：其局部小波功率谱服从χ22分布.在此基础上,利用假设检验给出了在给定置信度下确定有效信号在小波变换域内能量分布空间的方法,通过在有效信号能量分布空间重建信号来压制噪声.给出了模型及实际地震资料算例,证明了本文提出的方法的有效性.  相似文献   

邢台地区新近沉积粉质粘土的土性分析   总被引：3，自引：0，他引：3  

高俊良 《煤田地质与勘探》1997,25(2):40-42

以邢台地区新近沉积粉质粘土为例,对其土性进行分析,介绍了其在SEM下观察及X－射线衍射分析结果;并对该土的地基评价与处理方法进行了探讨。   相似文献   

矿物和玻璃中MgK-边X射线吸收光谱研究   总被引：1，自引：1，他引：0  

彭明生  李迪恩 《矿物岩石地球化学通报》1999,(4)

我们利用同步辐射Ｘ射线吸收光谱已经研究了硅酸盐矿物、铝硅酸盐矿物和玻璃中的主要阴离子Ｓｉ、ＡｌＫ边Ｘ射线吸收光谱［１～５］,指出随着压力变化而引起Ｓｉ、ＡｌＫ边向高能位移而配位数增大的规律。硅由４配位（如石英）变成６配位（如柯石英）。Ａｌ在矿物结构中的配位不同,如４配位的蓝晶石、５配位的红柱石、６配位的矽线石。这些矿物的局部结构不同,其键长、键角也不同,从而引起矿物的物理性质发生明显的变化。Ｍｇ不仅是地壳中广泛分布的造岩元素,而且也是组成地幔物相和未分异的原始岩浆的主要成分,是组成造岩矿物的…  相似文献