Observations of the first light and the epoch of reionization     

Xiaohui Fan 《天体物理学报》2012,(8):865-890

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A numerical study of self-gravitating protoplanetary disks     

Kazem Faghei 《天体物理学报》2012,(3):331-344

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Orbital effects of non-isotropic mass depletion of the atmospheres of evaporating hot Jupiters in extrasolar systems     

Lorenzo Iorio 《New Astronomy》2012,17(3):356-361

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The Torun catalogue of 6.7 GHz methanol masers     

M. Szymczak  P. Wolak  A. Bartkiewicz  K.M. Borkowski 《Astronomische Nachrichten》2012,333(7):634-639

We report the observations of 289 methanol maser sources at 6.7 GHz obtained over a two month period with the Torun 32 m telescope. The data form a catalogue of all objects north of δ = –22° brighter than 7.5 Jy in the peak emission. The positions of sub‐arcsecond accuracy are updated for 76 % of the objects. We find that about one third of the sources show changes in the peak fluxes by a factor of two or more on time scales of 8.5–9.5 years (© 2012 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

新型黏弹性阻尼器足尺性能试验研究          下载免费PDF全文

胡梅  张耀庭  孙江波  潘鹏 《地震工程学报》2021,43(1):238-244

黏弹性阻尼器是一种典型的被动控制装置,它可以通过黏弹性材料的剪切滞回耗能起到提高结构阻尼和减小结构地震或风振响应的作用。自主研发了损失系数不小于0.5的黏弹性材料,并基于此材料研发了新型国产黏弹性阻尼器。通过对黏弹性阻尼器足尺试件进行不同应变幅值、加载频率工况下的基本力学性能试验、以及低周疲劳性能试验,研究了不同工况下新型黏弹性阻尼器力学参数及其变化规律。试验结果表明:新型黏弹性阻尼器的损失系数在多数工况下处于0.3~0.4之间;其基本力学性能与加载频率相关性较小,随着应变幅值的增加表现出一定程度的软化特征,但在各应变幅值下均具有稳定的耗能能力;新型黏弹性阻尼器有良好的变形能力,在150%的应变下能保持稳定的基本力学性能,应变350%时仍未破坏;新型黏弹性阻尼器的疲劳性能较好,经低周疲劳加载后各项基本力学指标变化率均不超过25%。  相似文献   

基于Elman神经网络算法的地震经济损失快速评估研究     

郑韵  杨天青  王青平  郑超  朱耿青  魏娟 《中国地震》2021,37(3):610-619

地震经济损失快速评估是应急救灾的重要决策依据。本文选取了震级、极震区烈度、极震区烈度和抗震设防烈度之差ΔI、人口密度、人均GDP等5个指标作为输入层节点,将地震灾害的直接经济损失作为输出层节点,通过对1996—2013年的地震灾害损失资料进行训练和仿真分析,构建了Elman神经网络地震经济损失快速估计模型。运用该模型,对近年来的7个破坏性地震的直接经济损失进行评估分析,评估结果和实际直接经济损失有较好的一致性,该方法为地震经济损失快速评估提供了一种新思路。  相似文献   

Ore-Bearing Formations of the Precambrian in South China and Their Prospects     

HE Jurui  WANG Aiguo  RUI Xingjian  LI Chunhai Nanjing Institute of Geology  Mineral Resources  Nanjing  Jiangsu 《《地质学报》英文版》2004,78(2):375-379

In the Precambrian System of the Yangtze and Cathaysian plates six ore-bearing formations can be identified: the Cu-Pb-Zn-bearing formations in volcanic rocks of marine facies of the Neoarchean-Paleoproterozoic, Cu-Au-bearing formations and Pb-Zn-bearing formations in volcanic rocks of marine facies of the Mesoproterozoic, Pb-Zn-bearing formations in volcaniclastic rock and carbonate rock of the Neoproterozoic, Fe-Mn-bearing formations in the volcaniclastic rock of the Neoproterozoic, and Ni-Cr-serpentine-bearing formations in ophiolite and ultrabasic rock of the Meso- and Neoproterozoic. They were mostly formed in the marginal rift valleys of the Yangtze and Cathaysian plates, where occur stratabound and stratiform ore deposits, thermal deposits and porphyry polymetallic deposits. The six regions with ore-bearing formations have good prospects for ore deposits.  相似文献   

X‐rays from young stars: A summary of highlights from the XMM‐Newton Extended Survey of the Taurus Molecular Cloud (XEST)     

M. Güdel 《Astronomische Nachrichten》2008,329(2):218-221

The XMM‐Newton Extended Survey of the Taurus Molecular Cloud (XEST) is a survey of the nearest large star‐forming region, the Taurus Molecular Cloud (TMC), making use of all instruments on board the XMM‐Newton X‐ray observatory. The survey, presently still growing, has provided unprecedented spectroscopic results from nearly every observed T Tauri star, and from ≈50% of the studied brown dwarfs and protostars. The survey includes the first coherent statistical sample of high‐resolution spectra of T Tauri stars, and is accompanied by an U ‐band/ultraviolet imaging photometric survey of the TMC. XEST led to the discovery of new, systematic X‐ray features not possible before with smaller samples, in particular the X‐ray soft excess in classical T Tauri stars and the Two‐Absorber X‐ray (TAX) spectra of jet‐driving T Tauri stars. This paper summarizes highlights from XEST and reviews the key role of this large project. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

Observational signature of planet formation: The ALMA view     

Nagayoshi Ohashi 《Astrophysics and Space Science》2008,313(1-3):101-107

Protoplanetary disks are the most probable sites where planet formation takes place. According to theory, planet formation in protoplanetary disks should show remarkable signatures, such as a gap/hole or a spiral structure. In fact, recent high-angular and high-sensitivity observations in millimeter and submillimeter wavelengths, as well as optical/near-IR wavelengths, have shown such structures in protoplanetary disks. Two particular examples of such disks around AB Aurigae and HD 142527 are discussed here, with an emphasis on results obtained using the Submillimeter Array. These disks—and their probable planet formation—will be very important future targets for ALMA to study the physical process of planet formation in detail.  相似文献   

High-mass star forming regions: An ALMA view     

R. Cesaroni 《Astrophysics and Space Science》2008,313(1-3):23-28

The advent of ALMA is bound to improve our knowledge of OB star formation dramatically. Here, we present an overview of this topic outlining how high angular resolution and sensitivity may contribute to shed light on the structure of high-mass star forming regions and hence on the process itself of massive star formation. The impact of this new generation instrument will range from establishing the mass function of pre-stellar cores inside IR-dark clouds, to investigating the kinematics of the gas from which OB stars are built up, to assessing or ruling out the existence of circumstellar accretion disks in these objects.  相似文献