基于声波测试法对鹰滩页岩各向异性分析

页岩储层通常呈薄层状结构,一般认为其岩石力学参数具有横向各向同性,而其各向异性受围压（CP）、含水率和总有机质含量（TOC）等多种因素的影响。本文对不同围压下的鹰滩（Eagle Ford）页岩进行超声波波速进行测试实验,研究围压对鹰滩页岩波速及岩石力学各向异性的影响。实验结果表明,鹰滩页岩属于弱各向异性多孔介质,并具有横向各向同性、垂向各向异性的性质。纵波（P波）和横波（S波）波速随围压的增大而增大,特别是在低围压范围内增幅显著,同时围压增大会降低纵波和横波的各向异性,纵波各向异性比横波各向异性对围压更敏感。对鹰滩页岩各向异性分析为页岩储层压裂过程中裂缝的起裂和延伸规律研究提供了必要的力学参数。     

不同变形速率下前陆褶皱冲断带的发育特征——基于砂箱物理模拟实验研究

构造模拟实验是研究和模拟自然界地质构造现象、变形特征、成因机制和动力学过程的一种物理实验方法。本文基于砂箱构造物理模型高、中、低速7组不同单向挤压速度的构造模拟实验,揭示不同变形速率下砂箱物质变形的几何学、运动学及其演化特征,探讨不同变形速度(尤其是不同量级速度)对前陆褶皱冲断构造变形的重要性。高速单向挤压变形过程中(0.4~0.1mm/s),砂箱模型中石英砂体后缘构造加积强烈,砂体变形主要以楔形体向前扩展变形为主,其构造样式主要表现为前展式叠瓦冲断构造。中速挤压变形过程中(0.05~0.005mm/s),砂体后缘加积相对较弱,构造变形样式主要为砂箱楔形体前缘先形成(前展式为主)逆冲断层,当达到临界楔形体后,反冲断层发育并与前展式逆冲断层构成冲起构造,构造样式上表现为叠瓦构造与冲起构造的无序叠加。低速挤压变形过程中(0.002mm/s),砂箱物质构造样式以典型冲起带为主。由于砂箱模拟过程的时效性,即如何在最有效时间内获得最全面而复杂的演变过程,通过本次系列实验,我们建议将此有效挤压速度设定为0.05~0.005mm/s范围内,可以先后清晰而全面的获得高速和低速挤压下砂体的变形过程和构造样式。     

深部盐岩层绳索取心钻井液技术研究与应用

由于次生应力场的作用以及盐岩易溶于水的特性,深部盐岩层钻进存在岩层蠕动、钻井液易遭受盐钙侵等问题;钻进参数选择不合理易导致盐岩层取心效率低、岩心冲蚀严重。本文以河南省叶舞凹陷ZK3井为例,采用石油钻井与绳索取心相结合的措施,解决了普通固体矿产钻探设备在深部地层取心中效力不足的问题;通过阳离子交换容量测定、矿物组分鉴定、钻井液体系优选及性能测试等试验,确定了针对上部泥岩地层的聚合物钻井液体系,中部含膏泥岩的欠饱和盐水钻井液体系,下部盐岩层取心段的饱和盐水钻井液体系。通过确定合适的钻井液密度与临界环空返速,可以有效控制深部盐岩层蠕变与井壁冲蚀,适度提高排量以成倍提高钻进速度。钻进过程中钻井液性能稳定,体系转换顺利且性能易于调整,为取心任务的顺利完成提供了有力保证。     

下沉剂沉降堵水规律的研究

根据苏里格西区上气下水型储层的气水分布特征,该区适合下沉剂堵水压裂工艺。目前常用的下沉剂控缝高技术是在压裂时先将下沉剂通过携带液带入裂缝,随着下沉剂的下沉在裂缝的尖端处形成低渗透或不渗透的人工隔层,增加裂缝末梢的阻抗值,降低裂缝尖端的扩展应力,从而有效控制裂缝的垂向延伸。因此研究下沉剂在牛顿流体、非牛顿流体及裂缝内的沉降规律,通过合理的工艺优化设计,有利于提高堵水增气的效果。     

比例射线移位算法的改进及其应用

点状要素群移位的比例射线算法能够较好地保持移位后点群的空间分布模式。文中从农村居民地群移位的实际要求出发,对比例射线移位算法进行了改进:首先考虑居民地面积的不同大小对移位的影响;其次,设计比例射线移位的迭代方法;最后对于非常邻近的居民地群的移位,采用"微小"移位方法。通过实验验所改进的算法是有效的。     

GPS-RTK无验潮测深精度影响因素分析

针对目前GPS-RTK联合单波束无验潮测深虽然从理论上消除了潮位模型误差的影响,但未顾及测量船受风浪、海流、潮汐等作用引起的姿态影响、GPS与测深仪信号不同步的影响、测深仪信号延迟和水中声速变化的影响等问题,为了提高海洋测深成果的精度,文章在分析这些影响因素产生机理的基础上,结合当前常用的外业作业设备,仿真模拟了各种测深作业状况,并分别定量计算了各种状况下上述因素引起的定位和测深误差,然后依据分析计算结果,给出了相应的解决办法,可为测深外业作业人员区分误差量级,进而优化作业方案提供参考。     

Assessment of the Evolution in Velocity of Two Debris‐Covered Valley Glaciers in Nepal and New Zealand

Feature tracking of orthorectified pairs of Advanced Spaceborne Thermal Emission and Reflection Radiometer satellite images is used to calculate velocities for the Tasman Glacier, New Zealand (2002–2014) and the Khumbu Glacier, Nepal (2001–2008). Velocities in the middle and upper ablation zones of both glaciers show a long‐term decrease of ～10–20%, while the terminus of Khumbu Glacier has remained near stagnation throughout the study period. In contrast, there has been a recent acceleration of the lower terminus of Tasman Glacier, from ～5 m a^–1 in 2002 to 40 m a^–1 in 2014. Both of these glaciers have an extensive supraglacial debris cover across their lower ablation regions, with the Khumbu Glacier terminating on land and the Tasman Glacier terminating in a proglacial lake. The rapid recent increase in velocity of the terminus of Tasman Glacier is closely correlated with the increase in size of its proglacial lake. These results indicate the complex dynamic changes that mountain valley glaciers may undergo in response to long‐term negative mass balance.     

核电厂设计基准风速计算有关问题探讨

设计基准风速的确定对核电厂建构筑物的风荷载设计和结构设计至关重要。利用气象台站积累的历史极端风速资料,计算核电厂设计基准风速,并讨论了计算过程中应注意的有关问题。     

Time‐series high‐resolution spectroscopy and photometry of ε Aurigae from 2006–2013: Another brick in the wall

We present continuous and time‐resolved R = 55 000 optical échelle spectroscopy of ε Aurigae from 2006–2013. Data were taken with the STELLA Echelle Spectrograph of the robotic STELLA facility at the Observatorio del Teide in Tenerife. Contemporaneous photometry with the Automatic Photoelectric Telescopes at Fairborn Observatory in Arizona is presented for the years 1996–2013. Spectroscopic observations started three years prior to the photometric eclipse and are still ongoing. A total of 474 high‐resolution échelle spectra are analyzed and made available in this paper. We identify 368 absorption lines of which 161 lines show the characteristic sharp disk lines during eclipse. Another 207 spectral lines appeared nearly unaffected by the eclipse. From spectrum synthesis, we obtained the supergiant atmospheric parameters T_eff = 7395 ± 70 K, log g ≈ 1, and [Fe/H] = +0.02 ± 0.2 with ξ_t = 9 km s^–1, ζ_RT = 13 km s^–1, and v sin i = 28 ± 3 km s^–1. The residual average line broadening expressed in km s^–1 varies with a period of 62.6 ± 0.7 d, in particular at egress and after the eclipse. Two‐dimensional line‐profile periodograms show several periods, the strongest with ≈110 d evident in optically thin lines as well as in the Balmer lines. Center‐of‐intensity weighted radial velocities of individual spectral lines also show the 110‐d period but, again, additional shorter and longer periods are evident and are different in the Balmer lines. The two main spectroscopic Hα periods, ≈ 116 d from the line core and ≈ 150 d from the center‐of‐intensity radial velocities, appear at 102 d and 139 d in the photometry. The Hβ and Johnson V I photometry on the other hand shows two well‐defined and phase‐coherent periods of 77 d and 132 d. We conclude that Hα is contaminated by changes in the circumstellar environment while the Hβ and V I photometry stems predominantly from the non radial pulsations of the F0 supergiant. We isolate the disk‐rotation profile from 61 absorption lines and found that low disk eccentricity generally relates to low disk rotational velocity (but not always) while high disk eccentricity always relates to high velocity. There is also the general trend that the disk‐absorption in spectral lines with higher excitation potential comes from disk regions with higher eccentricity and thus also with higher rotational velocity. The dependency on transition probability is more complex and shows a bi‐modal trend. The outskirts of the disk is distributed asymmetrically around the disk and appears to have been built up mostly in a tail along the orbit behind the secondary. Our data show that this tail continues to eclipse the F0 Iab primary star even two years after the end of the photometric eclipse. High‐resolution spectra were also taken of the other, bona‐fide, visual‐binary components of ε Aur (ADS 3605BCDE). Only the C‐component, a K3‐4‐giant, appears at the same distance than ε Aur but its radial velocity is in disagreement with a bound orbit. The other components are a nearby (≈ 7 pc) cool DA white dwarf, a G8 dwarf, and a B9 supergiant, and not related to ε Aur. The cool white dwarf shows strong DIB lines that suggest the existence of a debris disk around this star. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

The Subaru Telescope High Dispersion Spectrograph (HDS)

The High Dispersion Spectrograph (HDS) is the échelle spectrograph for an open‐use instrument of the Subaru Telescope. The current status of the instrument is reviewed. The new image slicers that significantly improve the efficiency of observations with very high resolving power have been installed in the past three years. Brief overview of recent science results is given on studies of early generations of stars and extra‐solar planets. An upgrade plan and future prospects of this instrument are discussed. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)