半无限含水层中带衬砌隧洞渗流解析研究   总被引：3，自引：0，他引：3  

童磊  谢康和  卢萌盟  王坤 《岩土力学》2011,32(1):304-308

现有关于半无限含水层中隧洞渗流的解析解不能考虑衬砌部分排水的特性。假定土体和衬砌均为饱和均匀连续介质,采用土体与衬砌分算;利用复变函数解决孔口问题基本方法,对土体采用共形映射坐标变换,将土体中的渗流方程转换为与衬砌部分类似的二维Laplace方程圆环域的Dirichlet问题;通过Fourier解法,根据边界条件并利用流量连续条件,求得半无限空间中带衬砌隧洞渗流量和衬砌周边水头解析解答。分析了径深比、土体与衬砌渗透系数相对值、内壁水压力等因素对渗流量和衬砌周边水头的影响,并与数值算例进行了比较。结果表明,对浅埋隧洞该解析解仍具有较好的精度,是简便、实用的计算方法。  相似文献   

VisualModflow模型在白涧铁矿区矿井涌水量预测中的应用   总被引：1，自引：1，他引：0  

冯更辰  郝俊杰  谭俊  徐素娟 《中国岩溶》2011,30(3):271-277

在分析确定白涧矿区水文地质边界条件的基础上,运用实测资料对Visu-almodflow模型进行识别和验证,同时修正了含水层的参数,修正后的模型较为可靠,可用于白涧矿区涌水量的预测。依据矿区奥灰含水层边界条件和渗透系数的不同,设计了-200m和-400m水平面不同边界及渗透系数三个方案对矿井的涌水量进行预测。结果表明:方案2的涌水量比较合理,能较真实的反映白涧铁矿矿体分布区水位疏降至-400m时的涌水量情况,预测其涌水量为7505m3/h。   相似文献   

Hazards from pyroclastic density currents at Mt. Etna (Italy)     

Boris Behncke   《Journal of Volcanology and Geothermal Research》2009,180(2-4):148

Despite the recent recognition of Mount Etna as a periodically violently explosive volcano, the hazards from various types of pyroclastic density currents (PDCs) have until now received virtually no attention at this volcano. Large-scale pyroclastic flows last occurred during the caldera-forming Ellittico eruptions, 15–16 ka ago, and the risk of them occurring in the near future is negligible. However, minor PDCs can affect much of the summit area and portions of the upper flanks of the volcano. During the past ~ 20 years, small pyroclastic flows or base-surge-like vapor and ash clouds have occurred in at least 8 cases during summit eruptions of Etna. Four different mechanisms of PDC generation have been identified during these events: (1) collapse of pyroclastic fountains (as in 2000 and possibly in 1986); (2) phreatomagmatic explosions resulting from mixing of lava with wet rock (2006); (3) phreatomagmatic explosions resulting from mixing of lava with thick snow (2007); (4) disintegration of the unstable flanks of a lava dome-like structure growing over the rim of one of the summit craters (1999). All of these recent PDCs were of a rather minor extent (maximum runout lengths were about 1.5 km in November 2006 and March 2007) and thus they represented no threat for populated areas and human property around the volcano. Yet, events of this type pose a significant threat to the lives of people visiting the summit area of Etna, and areas in a radius of 2 km from the summit craters should be off-limits anytime an event capable of producing similar PDCs occurs. The most likely source of further PDCs in the near future is the Southeast Crater, the youngest, most active and most unstable of the four summit craters of Etna, where 6 of the 8 documented recent PDCs originated. It is likely that similar hazards exist in a number of volcanic settings elsewhere, especially at snow- or glacier-covered volcanoes and on volcano slopes strongly affected by hydrothermal alteration.  相似文献   

北极加拿大海盆2003年和2008年上层海洋热含量的差异分析   总被引：1，自引：0，他引：1       下载免费PDF全文

钟文理  赵进平 《极地研究》2012,24(1):24-34

主要利用2003年和2008年两次夏季北极科学考察的CTD数据处理了加拿大海盆上层海洋的热含量(这里上层海洋指的是200m以上的海洋),定量分析了热含量随深度的变化,并比较分析了这两年在夏季海冰融化期间热含量的垂向差异变化,以及影响热含量变化的因素,给出了上层海洋热含量在加拿大海盆的空间分布。2008年与2003年相比最显著的变化是在加拿大海盆开阔水域的增加,这将导致太阳辐射能进入海洋中的能量增加,同时海冰的大量融化带来了大量淡水,这些变化改变了上层海洋的温盐性质。海冰大量融化主要产生两个效应：一是上层海洋的普遍增暖,二是太平洋入流水体的下移。文中还分析了近年来在加拿大海盆中变化显著的次表层暖水现象,由于次表层暖水蕴含着不小的热含量,其在上层海洋热量平衡中的作用不容忽视。  相似文献   

云南省官房铅锌钨矿区团山矿段水文地质特征与矿区涌水量预测     

方娜  张世涛  程先锋  刘伟 《地质与资源》2015,24(6):583-586

官房铅锌钨矿区团山矿段位于云南省文山州文山县内,钨矿矿体规模中等,矿区水文地质条件中等偏复杂,包含有3个含水层组.矿坑充水的主要来源是矿体顶底板围岩岩溶裂隙水中的地下水.利用大井法对矿区的涌水量进行预测,结果表明1200、1300和1400 m水平段正常涌水量分别为21587、9997和4484 m³/d,最大涌水量分别为64761、29991和13452 m³/d.  相似文献   

Measuring the accretion rate and kinetic luminosity functions of supermassive black holes     

E. G. Körding  S. Jester  R. Fender 《Monthly notices of the Royal Astronomical Society》2008,383(1):277-288

We derive accretion rate functions (ARFs) and kinetic luminosity functions (KLFs) for jet-launching supermassive black holes. The accretion rate as well as the kinetic power of an active galaxy is estimated from the radio emission of the jet. For compact low-power jets, we use the core radio emission while the jet power of high-power radio-loud quasars is estimated using the extended low-frequency emission to avoid beaming effects. We find that at low luminosities the ARF derived from the radio emission is in agreement with the measured bolometric luminosity function (BLF) of active galactic nucleus (AGN), i.e. all low-luminosity AGN launch strong jets. We present a simple model, inspired by the analogy between X-ray binaries (XRBs) and AGN, that can reproduce both the measured ARF of jet-emitting sources as well as the BLF. The model suggests that the break in power-law slope of the BLF is due to the inefficient accretion of strongly sub-Eddington sources. As our accretion measure is based on the jet power it also allows us to calculate the KLF and therefore the total kinetic power injected by jets into the ambient medium. We compare this with the kinetic power output from supernova remnants (SNRs) and XRBs, and determine its cosmological evolution.  相似文献   

Fossil AGN jets as ultrahigh-energy particle accelerators     

Gregory Benford  R. J. Protheroe 《Monthly notices of the Royal Astronomical Society》2008,383(2):663-672

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Erratum: Luminosity function, sizes and FR dichotomy of radio-loud AGN     

《Monthly notices of the Royal Astronomical Society》2008,384(4):1742-1742

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High-energy afterglow emission from gamma-ray bursts     

Yi-Zhong Fan †  Tsvi Piran †  Ramesh Narayan †  Da-Ming Wei † 《Monthly notices of the Royal Astronomical Society》2008,384(4):1483-1501

We calculate the very high-energy (sub-GeV to TeV) inverse Compton emission of GRB afterglows. We argue that this emission provides a powerful test of the currently accepted afterglow model. We focus on two processes: synchrotron self-Compton emission within the afterglow blast wave, and external inverse Compton emission which occurs when flare photons (produced by an internal process) pass through the blast wave. We show that if our current interpretations of the Swift X-ray telescope (XRT) data are correct, there should be a canonical high-energy afterglow emission light curve. Our predictions can be tested with high-energy observatories such as GLAST , Whipple, HESS and MAGIC. Under favourable conditions we expect afterglow detections in all these detectors.  相似文献   

A deep X-ray observation of M82 with XMM–Newton     

P. Ranalli †‡  A. Comastri  L. Origlia  R. Maiolino § 《Monthly notices of the Royal Astronomical Society》2008,386(3):1464-1480

We report on the analysis of a deep (100-ks) observation of the starburst galaxy M82 with the EPIC and RGS instruments onboard the X-ray telescope XMM–Newton . The broad-band (0.5–10 keV) emission is due to at least three spectral components: (i) continuum emission from point sources; (ii) thermal plasma emission from hot gas; and (iii) charge-exchange emission from neutral metals (Mg and Si). The plasma emission has a double-peaked differential emission measure, with the peaks at ∼0.5 and ∼7 keV. Spatially resolved spectroscopy has shown that the chemical absolute abundances are not uniformly distributed in the outflow, but are larger in the outskirts and smaller close to the galaxy centre. The abundance ratios also show spatial variations. The X-ray-derived oxygen abundance is lower than that measured in the atmospheres of red supergiant stars, leading to the hypothesis that a significant fraction of oxygen ions have already cooled off and no longer emit at energies ≳0.5 keV.  相似文献