广西向阳坪铀矿床钻探施工技术及改进措施

广西向阳坪铀矿床岩性以花岗岩为主,研磨性强,部分地层复杂,构造裂隙密集发育,岩石破碎,绿泥石化、高岭土化强烈,钻探施工困难。通过采用金刚石绳索取心钻探技术和施工工艺,并针对钻进中遇到的问题,引进了便携式全液压钻机,采用了成膜防塌无固相冲洗液体系及延迟交联凝胶堵漏工艺,优选了环齿式孕镶金刚石钻头,并采取了严格的预防和控制防斜措施,解决了钻进效率低、孔壁不稳定、金刚石钻头寿命短及钻孔弯曲等一系列问题。生产实践证明,该施工技术和工艺具有钻进效率高、岩（矿）心采取率高、劳动强度低等优点,可为花岗岩及复杂岩层钻进施工提供借鉴。     

钻探技术在矿山灾害事故应急救援中的应用

钻探作为一种有效的应急救援手段在矿山灾害事故应急救援工作中得到了应用。本文根据应用目标不同将应急救援钻孔分为生命保障孔、救生孔、排水孔、灭火孔、瓦斯抽放孔等。生命保障孔钻探技术、排水孔钻探技术、大口径救生孔钻探技术等3种典型的矿山灾害事故应急救援钻探技术在矿山灾害应急救援工作中得到成功应用,取得了不错的效果。加强矿山灾害事故应急救援钻探技术配套设备的研发和相关钻探工艺研究将有力促进矿山灾害事故应急救援的发展。     

2014年南京两次弱降雪过程的对比分析

利用常规观测资料和NCEP再分析资料,结合多普勒雷达等资料,对2014年2月9—10日江苏大部分地区出现的两次弱降雪过程进行了成因分析。结果表明:9日的降雪是由中层西风槽东移影响,槽前西南暖湿气流在低层冷空气垫上爬升所致,是一次层状云降雪;10日的降雪则是低空冷空气主体偏北东移,内陆偏西地区低空风速随之明显减小,而东部沿海地区风速变化不大,从而使得辐合上升区西扩所致;10日低空上升运动带来的低云降雪,尺度小,且具有类似弱对流系统的特征。常规业务中使用的数值预报产品(如EC)并不能准确预报这两次弱降雪过程,特别是10日过程预报效果较差,而WRF模式则对10日过程把握较好。     

Black hole spin dependence of general relativistic multi-transonic accretion close to the horizon

We introduce a novel formalism to investigate the role of the spin angular momentum of astrophysical black holes in influencing the behavior of low angular momentum general relativistic accretion. We propose a metric independent analysis of axisymmetric general relativistic flow, and consequently formulate the space and time dependent equations describing the general relativistic hydrodynamic accretion flow in the Kerr metric. The associated stationary critical solutions for such flow equations are provided and the stability of the stationary transonic configuration is examined using an elegant linear perturbation technique. We examine the properties of infalling material for both prograde and retrograde accretion as a function of the Kerr parameter at extremely close proximity to the event horizon. Our formalism can be used to identify a new spectral signature of black hole spin, and has the potential of performing the black hole shadow imaging corresponding to the low angular momentum accretion flow.     

Magnetic field and radius of the innermost stable circular orbit near super‐massive black holes in active galactic nuclei

Magnetic fields in an accretion disk around the central black hole can modify the size of the innermost stable circular orbit (ISCO) and can produce a difference to the classical Novikov‐Thorne radius. We estimated the ISCO magnetic field strength from the polarimetric observations of the accretion‐disk radiation. This estimate is obtained taking into account the effect of the Faraday rotation of the polarization plane at the distance of the mean free path of photons between successive electron scattering events. We present the new method for estimating the ISCO radius in the accretion disk, i.e. in the nearest vicinity of a central black hole. Our estimates confirmed the Frolov, Shoom & Tzounis (2014) and Ranea‐Sandoval & Garcia (2015) conclusion that the magnetic field in the accretion disk decreases the size of the innermost stable circular orbit. (© 2015 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Geometry of scour hole around, and the influence of the angle of attack on the burial of finite cylinders under combined flows

Experiments were conducted to investigate the geometry of the scour hole and flow structure around short cylinders under the action of waves alone (WA) and combined flows (CF). The study is aimed at better understanding the dynamics of isolated objects on a sandy floor under oscillatory flows as occurs in shallow water regions in coastal areas. Flow velocities within the fluid core were recorded and 3D mapping of the bottom was performed with sub-aquatic acoustic sensors. Experiments were conducted for cylinder Reynolds wave number and Keulegan-Carpenter number within the ranges 10⁴R_e1.7×10⁵ and 2KC71, respectively. The present experimental evidence shows that the geometric characteristics of the scour hole (length and width) depend primarily on the Keulegan-Carpenter number (KC) and the cylinder aspect ratio (a_r=L_c/D). The effect of variation in the angle of attack of the flow with respect to the cylinder main axis was also investigated. Initial orientations of zero and ninety degrees were found to be stable while cylinders with intermediate initial orientations tended to orientate their main axes perpendicular to the flow direction. The final angle of orientation was found to be primarily a function of the Shields parameter, θ, and the initial angle of attack, α_i.     

Back reaction and Hawking radiation from a Vaidya black hole

Using Damour-Ruffini’s and Hamilton-Jacobi’s methods, Hawking radiation from a Vaidya black hole is investigated. Due to non-stationary black holes, the event horizon r _H and the entropy S are all related to both the mass m(υ) and . When the back-reaction of particles’s energy to space-time is considered, we get the emission probability. It is found that the result is different from that of the stationary Schwarzschild black hole, because is the function of mass m(υ).      

Gravitational waves from resolvable massive black hole binary systems and observations with Pulsar Timing Arrays

Massive black holes are key components of the assembly and evolution of cosmic structures, and a number of surveys are currently on going or planned to probe the demographics of these objects and to gain insight into the relevant physical processes. Pulsar Timing Arrays (PTAs) currently provide the only means to observe gravitational radiation from massive black hole binary systems with masses  ≳10⁷ M_⊙  . The whole cosmic population produces a stochastic background that could be detectable with upcoming PTAs. Sources sufficiently close and/or massive generate gravitational radiation that significantly exceeds the level of the background and could be individually resolved. We consider a wide range of massive black hole binary assembly scenarios, investigate the distribution of the main physical parameters of the sources, such as masses and redshift, and explore the consequences for PTAs observations. Depending on the specific massive black hole population model, we estimate that on average at least one resolvable source produces timing residuals in the range  ∼5–50 ns  . PTAs, and in particular the future Square Kilometre Array, can plausibly detect these unique systems, although the events are likely to be rare. These observations would naturally complement on the high-mass end of the massive black hole distribution function future surveys carried out by the Laser Interferometer Space Antenna .