Assessing the Vibrational Frequencies of the Holweide Hospital in the City of Cologne (Germany) by Means of Ambient Seismic Noise Analysis and FE modelling     

Stefano?ParolaiEmail author  Andreas?F?cke  Sandra?M.?Richwalski  Lothar?Stempniwski 《Natural Hazards》2005,34(2):217-230

Ambient seismic noise measurements were conducted inside the Holweide Hospital (Cologne) for checking whether its frequencies of vibration fall into the range where soil amplification is expected. If this is the case, damage might increase in case of an earthquake due to an amplified structural response of the building. Two different techniques were used: the ratio between the horizontal and vertical components of the spectra recorded at stations located inside the building and the ratio between the corresponding components of the spectra recorded simultaneously inside the building and at a reference station placed outside. While the former method might be preferred because of less equipment involved, the latter has the advantage of producing more stable results and deleting automatically the influence of the sedimentary cover, which might obscure some eigenfrequencies of vibration of the building. An independently performed finite-element analysis of the hospital showed a good correlation between measured and calculated eigenmodes.  相似文献   

An interacting O + O supergiant close binary system: Cygnus OB2-5 (V729 Cyg)     

《New Astronomy》2014

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New magnetic field measurements of β Cephei stars and slowly pulsating B stars     

S. Hubrig  M. Briquet  P. De Cat  M. Schller  T. Morel  I. Ilyin 《Astronomische Nachrichten》2009,330(4):317-329

We present the results of the continuation of our magnetic survey with FORS 1 at the VLT of a sample of B‐type stars consisting of confirmed or candidate β Cephei stars and Slowly Pulsating B (hereafter SPB) stars, along with a small number of normal B‐type stars. A weak mean longitudinal magnetic field of the order of a few hundred Gauss was detected in three β Cephei stars and two stars suspected to be β Cephei stars, in five SPB stars and eight stars suspected to be SPB stars. Additionally, a longitudinal magnetic field at a level larger than 3σ has been diagnosed in two normal B‐type stars, the nitrogen‐rich early B‐type star HD 52089 and in the B5 IV star HD 153716. Roughly one third of β Cephei stars have detected magnetic fields: Out of 13 β Cephei stars studied to date with FORS 1, four stars possess weak magnetic fields, and out of the sample of six suspected β Cephei stars two show a weak magnetic field. The fraction of magnetic SPBs and candidate SPBs is found to be higher: Roughly half of the 34 SPB stars have been found to be magnetic and among the 16 candidate SPBs eight stars possess magnetic fields. In an attempt to understand why only a fraction of pulsating stars exhibit magnetic fields, we studied the position of magnetic and non‐magnetic pulsating stars in the H‐R diagram. We find that their domains in the H‐R diagram largely overlap, and no clear picture emerges as to the possible evolution of the magnetic field across the main sequence. It is possible that stronger fields tend to be found in stars with lower pulsating frequencies and smaller pulsating amplitudes. A somewhat similar trend is found if we consider a correlation between the field strength and the v sin i ‐values, i.e. stronger magnetic fields tend to be found in more slowly rotating stars (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

57-second oscillations in Nova Centauri 1986 (V842 Cen)     

Patrick A. Woudt  Brian Warner  Julian Osborne  Kim Page 《Monthly notices of the Royal Astronomical Society》2009,395(4):2177-2182

High-speed photometry in 2008 shows that the light curve of V842 Cen possesses a coherent modulation at 56.825 s, with sidebands at 56.598 and 57.054 s. These have appeared since this nova remnant was observed in 2000 and 2002. We deduce that the dominant signal is the rotation period of the white dwarf primary and the sidebands are caused by reprocessing from a surface moving with an orbital period of 3.94 h. Thus, V842 Cen is an intermediate polar (IP) of the DQ Herculis subclass, is the fastest rotating white dwarf among the IPs and is the third fastest known in a cataclysmic variable. As in other IPs, we see no dwarf nova oscillations, but there are often quasi-periodic oscillations in the range 350–1500 s. There is a strong brightness modulation with a period of 3.78 h, which we attribute to negative superhumps, and there is an even stronger signal at 2.886 h which is of unknown origin but is probably a further example of that seen in GW Lib and some other systems. We used the Swift satellite to observe V842 Cen in the ultraviolet and in X-rays, although no periodic modulation was detected in the short observations. The X-ray luminosity of this object appears to be much lower than that of other IPs in which the accretion region is directly visible.  相似文献   

Detection and evolution of the CO (Δv= 2) emission in Nova V2615 Ophiuchi (2007)     

R. K. Das  D. P. K. Banerjee  N. M. Ashok 《Monthly notices of the Royal Astronomical Society》2009,398(1):375-384

We present near-infrared (1–2.5 μm) spectroscopic and photometric results of Nova V2615 Ophiuchi which was discovered in outburst in 2007 March. Our observations span a period of ∼80 d starting from 2007 March 28 when the nova was at its maximum light. The evolution of the spectra is shown from the initial P Cygni phase to an emission-line phase and finally to a dust formation stage. The characteristics of the JHK spectra are very similar to those observed in a nova outburst occurring on a carbon–oxygen white dwarf. We analyse an observed line at 2.088 μm and suggest that it could be due to Fe  ii excited by Lyman α fluorescence. The highlight of the observations is the detection of the first overtone bands of carbon monoxide (CO) in the 2.29–2.40 μm region. The CO bands are modelled to estimate the temperature and mass of the emitting CO gas and also to place limits on the ¹²C/¹³C ratio. The CO bands are recorded over several epochs, thereby allowing a rare opportunity to study the evolution from a phase of constant strength through a stage when the CO is destroyed fairly rapidly. We compare the observed time-scales involved in the evolution of the CO emission and find a good agreement with model predictions that investigate the chemistry in a nova outflow during the early stages.  相似文献   

河北承德大庙黑山钒钛磁体矿床地质特征与成因探讨   总被引：8，自引：1，他引：7  

孙静  杜维河  王德忠  李健  徐国新  韩玉丑 《地质学报》2009,83(9):1344-1364

河北承德大庙黑山铁矿床位于大庙斜长岩体南部边缘,红石砬—大庙深断裂附近北侧。矿区内主要岩类为斜长岩,根据蚀变作用可分为钠黝帘石化斜长岩、绿泥石化斜长岩及混染斜长岩等,前者广泛分布于矿区内,后二者常构成铁矿的直接围岩。黑山铁矿苏长岩体与铁矿体有成因联系,主要受近东西向压扭性断层和龙潭沟—岔沟压扭性断裂带构造控制,分布于黑山斜长岩体内。部分苏长岩体中有分异式浸染矿体,在苏长岩接触带及其围岩中的矿体则为贯入式矿体。苏长岩体根据其特征和共生组合,可划分为两个岩石系列：①苏长岩岩石系列（苏长岩类型岩体、含橄苏长岩苏长岩类型岩体）;②二长岩苏长岩岩石系列（二长岩苏长岩类型岩体、二长岩橄榄苏长岩类型岩体）。矿石结构主要为自形—半自形晶粒状结构、格状熔离结构、海绵陨铁结构。矿石构造有致密块状构造、浸染状构造。矿石金属矿物主要为含钒钛磁铁矿（含量3%～60%）、钛铁矿（含量2%～19%）、含钒磁铁矿（含量7%～27%）,次有少量含钴黄铁矿、黄铜矿。脉石矿物主要为绿泥石（含量7%～33%）,次为斜长石（0%～45%）,及其它少量矿物。黑山的矿源苏长岩和中国及世界同类岩石有显著不同,Si、Al、Fe、Ti、P、Na、K含量高,Ca、Mg含量低,这类岩体为形成铁磷矿床提供了物质来源。本区斜长岩、矿源苏长岩铁矿床和铁磷矿床的氧同位素组成δ18O限于一个很窄的变化范围,反映了它们的物质来源和成因类型的同一性。黑山苏长岩、伟晶苏长岩δ34S 为+1.3‰～+2.1‰,反映苏长岩浆来源于上地幔。黑山铁磷矿体经铁钛氧化物矿物对形成温度计计算得出生成温度为615~975℃,显示该岩浆矿床高温成矿特点。研究认为黑山铁矿主要①、②号铁矿体为岩浆贯入成矿。  相似文献   

Breakdown of hydrous ringwoodite to pyroxene and spinelloid at high P and T and oxidizing conditions     

M. Koch-Müller  D. Rhede  R. Schulz  R. Wirth 《Physics and Chemistry of Minerals》2009,36(6):329-341

To get deeper insight into the phase relations in the end-member system Fe₂SiO₄ and in the system (Fe, Mg)₂SiO₄ experiments were performed in a multi-anvil apparatus at 7 and 13 GPa and 1,000–1,200°C as a function of oxygen fugacity. The oxygen fugacity was varied using the solid oxygen buffer systems Fe/FeO, quartz–fayalite–magnetite, MtW and Ni/NiO. The run products were characterized by electron microprobe, Raman- and FTIR-spectroscopy, X-ray powder diffraction and transmission electron microscopy. At fO₂ corresponding to Ni/NiO Fe-ringwoodite transforms to ferrosilite and spinelloid according to the reaction: 9 Fe₂SiO₄ + O₂ = 6 FeSiO₃ + 5 Fe_2.40Si_0.60O₄. Refinement of site occupancies in combination with stoichiometric Fe³⁺ calculations show that 32% of the total Fe is incorporated as Fe³⁺ according to From the Rietveld refinement we identified spl as spinelloid III (isostructural with wadsleyite) and/or spinelloid V. As we used water in excess in the experiments the run products were also analyzed for structural water incorporation. Adding Mg to the system increases the stability field of ringwoodite to higher oxygen fugacity and the spinel structure seems to accept higher Fe³⁺ but also water concentrations that may be linked. At oxygen fugacity corresponding to MtW conditions similar phase relations in respect to the breakdown reaction in the Fe-end-member system were observed but with a strong fractionation of Fe into spl and Mg into coexisting cpx. Thus, through this strong fractionation it is possible to stabilize very Fe-rich wadsleyite with considerable Fe³⁺ concentrations even at an intermediate Fe–Mg bulk composition: assuming constant K _D independent on composition and a bulk composition of x _Fe = 0.44 this fractionation would stabilize spl with x _Fe = 0.72. Thus, spl could be a potential Fe³⁺ bearing phase at P–T conditions of the transition zone but because of the oxidizing conditions and the Fe-rich bulk composition needed one would expect it more in subduction zone environments than in the transition zone in senso stricto.

M. Koch-MüllerEmail:

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Detection of superhumps in the cataclysmic variable V378 Peg (PG 2337+300)     

V.P. Kozhevnikov 《New Astronomy》2012,17(1):38-42

The cataclysmic variable V378 Peg is known since 15 years. Although V378 Peg is a rather bright star (14 mag), it underwent no detailed study. We performed photometric observations of V378 Peg during 75 h with the goal to detect periodic brightness variations. The obtained light-curves clearly showed changes with a period of about 3 h. The Fourier analysis reveals that this oscillation occurs with a period of 3.238 h and a semiamplitude of 0.07 mag. Although the detected oscillation possesses certain coherence, it appears to have a slightly unstable period or phase. Therefore, the detected period cannot be the orbital period of the V378 Peg system. Because such instability is typical of superhumps, we must consider the detected oscillation as superhumps. Furthermore, V378 Peg shows no outbursts and has to be a nova-like variable rather than a dwarf nova. Hence, the detected superhumps have to be regarded as permanent superhumps. Because superhump periods in cataclysmic variables are close to orbital periods, we can find the place of V378 Peg in the orbital period distribution of cataclysmic variables. V378 Peg is a permanent superhump system above the upper edge of the 2-3 h period gap in the orbital period distribution.  相似文献   

青藏高原东北侧冰雹微物理过程模拟研究   总被引：31，自引：15，他引：16  

康凤琴  张强  渠永兴  冀兰芝  郭学良 《高原气象》2004,23(6):735-742

以青藏高原东北侧及毗邻地区诱发冰雹灾害的东移短小切变线天气过程为研究背景,采用中国科学院大气物理研究所三维冰雹云分档模式,用MM5V3中尺度气象模式提供冰雹云模拟研究所需的环境大气状况,模拟研究了冰雹形成和增长的微物理过程。结果表明：模式再现了当时冰雹、大风及暴雨的实况;中尺度水分和动力条件是冰雹形成和增长的重要因素,它们决定了冰雹云的强度和冰雹的大小;冰雹形成和增长过程中的微物理过程决定了冰雹云的消亡,冰雹在空中形成的潜热释放延长了降雹的时间;云中冰雹发生、增长的主要区域和云内上升气流配合良好,是防雹消雹的主要范围。  相似文献   

Accretion disc in the massive V448 Cygni system     

G. Djura&#;evi&#;  I. Vince  T. S. Khruzina  E. Rovithis-Livaniou 《Monthly notices of the Royal Astronomical Society》2009,396(3):1553-1558

The UBV light curves of the early-type eclipsing binary V448 Cygni, obtained at the Abastumani Astrophysical Observatory from 1964 to 1967, are re-analysed here. The analysis was made assuming the presence of an accretion disc in the system, as inferred from the light-curve shape and spectroscopic characteristics of the system. The Roche model of a binary was used, containing a geometrically and optically thick accretion disc around the hotter and more massive star. By solving the inverse problem, the orbital elements and the physical parameters of the system components and of the accretion disc were estimated. This result is important for understanding the star formation and evolution processes in the systems with massive components.  相似文献