地铁隧洞带水作业施工技术

以在建的北京地铁十号线双井一劲松区间暗挖隧道为例，通过分析北京特殊地层在带水条件下单洞结构单线隧道台阶法的施工工艺，洞悉浅埋暗挖正台阶法施工中超前预加固、开挖时空顺序、台阶长度等工艺对围岩稳定性的影响程度。     

桩端土加固处理设计及检测方法的探讨

介绍了人工挖孔桩桩端土承载力不足进行旋喷桩处理的设计过程以及处理后检测过程中遇到的问题。桩端土处理设计可以遵循一般的地基处理设计方法和原则,并针对复合地基承载力检测和桩端土极限端阻力的检测中存在的差异和共同点,提出组合静载荷试验的思路和方法,并在工程中予以实施,并取得了较好的效果。     

钻孔灌注桩桩底沉渣压浆处理研究与应用

对桩底沉渣产生的原因、沉渣对灌注桩承载能力的影响以及沉渣的处理作了简要分析,讨论了灌注桩桩底压浆工艺的作用机理。重点结合实际工程介绍了该技术,经检测表明,灌注桩桩底压浆技术的使用有效地处理了沉渣,提高了桩的承载能力。     

挤土类桩的挤土效应及其防治方法

挤土效应是所有挤土类桩面临的共同问题，它可能造成临近建筑物破坏，地下管线断裂，道路隆起以及工程质量事故。依据挤土类桩挤土效应的形成机理，结合工程实例，提出了减少挤土效应的措施，如预钻排水孔、开挖防挤沟、设置观测点、控制压桩速度等措施，并根据施工地区不同的环境条件提出了合理的压桩顺序。     

帷幕灌浆在坝基防渗处理中的应用——以新疆乌什水水库为例

新疆乌什水水库为注入式水库。于1984年始修,总库容3850×104m3,灌溉下游农田。因坝基严重渗漏,2002年被新疆水利专家评为险库,对坝基需进行防渗帷幕灌浆处理。为此,设计和施工中确定了坝基防渗处理原则,从而探索出一套最佳的灌浆工艺。现场运用多种手段对灌浆质量进行全面检查,对施工全过程实施质量控制和跟踪监理,使施工的838个灌浆孔(总进尺25804.18m)的优良率达84.8%,7个固结灌浆单元和21个帷幕灌浆单元工程合格率达100%。固结灌浆和帷幕灌浆部分工程及坝基防渗帷幕单位工程均被评为优良工程。     

化学注浆治理巨厚表土层立井井壁漏水

煤矿立井由于各种原因经常发生井壁渗漏水,严重影响正常的煤矿安全生产。邱集煤矿副立井表土层厚320m,为巨厚表土层,发生渗水后,采用改性脲醛树脂浆材成功进行了破壁注浆处理,将井筒的涌水量由10m3/h降至0.3m3/h左右。同时,注浆时浆液形成的帷幕能达到加固地层,减少地层压缩沉降量,排除生产安全隐患,保护井桶的作用。     

深厚堆积体地层钻进工艺方法研究

太钢(集团)有限公司矿业公司峨口铁矿是一个从20世纪60年代就开始开采的老矿区,经过长期开采储量已严重不足。为了延长矿山寿命,需要进一步扩大勘探范围,在原有矿山周边地区进行勘探。最初采用岩心勘探钻机进行常规回转钻进加套管护壁,历时3个月。在上部堆积体地层最大钻孔深度达到约20m,再也无法继续钻进,使勘探工作被迫停止。针对深厚堆积体地层钻孔施工遇到的具体困难,介绍了风动潜孔锤双管跟管钻进在工程施工中的应用,在对深厚堆积体地层进行分析的基础上,探讨进行深厚堆积体地层钻孔施工的工艺方法及技术措施;在钻孔结构基础上选择钻孔设备及钻孔机具的一般原则,对深厚堆积体地层的钻孔工程施工具一定指导意义。     

A simple mass estimate for central black holes in cuspy galaxies

We argue that the temperature of the stellar phase is likely a monotically decreasing function of radius in the central regions of elliptical galaxies with cusps. We show that it requires the presence of a central mass concentration. An estimate of its minimum mass based on few parameters is given. This lower bound is consistent with current mass values of the central objects in galaxies derived from detailed models. This revised version was published online in July 2006 with corrections to the Cover Date.     

High-redshift galaxies, their active nuclei and central black holes

We demonstrate that the luminosity function of the recently detected population of actively star-forming galaxies at redshift z  = 3 and the B -band luminosity function of quasi-stellar objects (QSOs) at the same redshift can both be matched with the mass function of dark matter haloes predicted by standard variants of hierarchical cosmogonies for lifetimes of optically bright QSOs anywhere in the range 10⁶ to 10⁸ yr. There is a strong correlation between the lifetime and the required degree of non-linearity in the relation between black hole and halo mass. We suggest that the mass of supermassive black holes may be limited by the back-reaction of the emitted energy on the accretion flow in a self-gravitating disc. This would imply a relation of black hole to halo mass of the form M _bh ∝  v ⁵_halo ∝  M ^5/3_halo and a typical duration of the optically bright QSO phase of a few times 10⁷ yr. The high integrated mass density of black holes inferred from recent black hole mass estimates in nearby galaxies may indicate that the overall efficiency of supermassive black holes for producing blue light is smaller than previously assumed. We discuss three possible accretion modes with low optical emission efficiency: (i) accretion at far above the Eddington rate, (ii) accretion obscured by dust, and (iii) accretion below the critical rate leading to an advection-dominated accretion flow lasting for a Hubble time. We further argue that accretion with low optical efficiency might be closely related to the origin of the hard X-ray background and that the ionizing background might be progressively dominated by stars rather than QSOs at higher redshift.     

Line emission from accretion discs around black holes: the analytic approach

The broad X-ray iron line observed in many active galactic nuclei spectra is thought to originate from the accretion disc surrounding the putative supermassive black hole. We show here how to perform the analytical integration of the geodesic equations that describe the photon trajectories in the general case of a rotating black hole (Kerr metric), in order to write a fast and efficient numerical code for modelling emission line profiles from accretion discs.