The brightness of the galactic radio loops at 1420 MHz: Some indications for the existence of Loops V and VI

In this article we use 1420 MHz data to demonstrate the likely reality of Galactic radio Loops V and VI. We further estimate distances and spectral indices for both these and the four main radio loops. In the cases of Loops I–IV, radio spectral indices are calculated from the mean brightnesses at 1420 and 820/404 MHz. The spectral indices of Loops V and VI are obtained from T –T plots between 1420 and 408 MHz. Using the supernova remnant (SNR) hypothesis for the origin of radio loops, distances are calculated from the surface brightnesses and the angular diameters at 1420 MHz. We also study how results for brightnesses and distances of radio loops agree with current theories of SNR evolution. For this purpose, the ambient density and initial explosion energy of the loops are discussed. We also discuss applications of different Σ–D relations. The results obtained confirm a non‐thermal origin and nearby locations for the Galactic radio loops. Therefore, we have indications that they are very old SNRs that evolve in low ambient densities, with high initial explosion energies. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Automated probabilistic classification of transients and variables

There is an increasing number of large, digital, synoptic sky surveys, in which repeated observations are obtained over large areas of the sky in multiple epochs. Likewise, there is a growth in the number of (often automated or robotic) follow‐up facilities with varied capabilities in terms of instruments, depth, cadence, wavelengths, etc., most of which are geared toward some specific astrophysical phenomenon. As the number of detected transient events grows, an automated, probabilistic classification of the detected variables and transients becomes increasingly important, so that an optimal use can be made of follow‐up facilities, without unnecessary duplication of effort. We describe a methodology now under development for a prototype event classification system; it involves Bayesian and Machine Learning classifiers, automated incorporation of feedback from follow‐up observations, and discriminated or directed follow‐up requests. This type of methodology may be essential for the massive synoptic sky surveys in the future. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

The Monitor project: rotation of low-mass stars in the open cluster NGC 2547

We report on the results of an I -band time-series photometric survey of NGC 2547 using the MPG/ESO 2.2-m telescope with Wide Field Imager, achieving better than 1 per cent photometric precision per data point over  14 ≲ I ≲ 18  . Candidate cluster members were selected from a V versus V − I colour–magnitude diagram over  12.5 < V < 24  (covering masses from  0.9 M_⊙  down to below the brown dwarf limit), finding 800 candidates, of which we expect ∼330 to be real cluster members, taking into account contamination from the field (which is most severe at the extremes of our mass range). Searching for periodic variations in these gave 176 detections over the mass range  0.1 ≲ M /M_⊙≲ 0.9  . The rotation period distributions were found to show a clear mass-dependent morphology, qualitatively intermediate between the distributions obtained from similar surveys in NGC 2362 and 2516, as would be expected from the age of this cluster. Models of the rotational evolution were investigated, finding that the evolution from NGC 2362 to 2547 was qualitatively reproduced (given the uncertainty in the age of NGC 2547) by solid body and core-envelope decoupled models from our earlier NGC 2516 study without need for significant modification.     

青藏高原北部多温型山谷冰川不同海拔处冰温变化研究 ——以祁连山老虎沟12号冰川为例

冰川温度是表征冰川物理属性和响应气候变化的关键指标。2010年7月至2011年11月在祁连山老虎沟12号冰川积累区（5 040 m）、多年平衡线处（4 900 m）和消融区（4 550 m）开展了活动层（22 m深,1 m间隔）冰温连续观测。2011年10月在冰川积累区4 971 m处钻得165 m深孔获取了115 m深层冰温廓线。研究发现：三个区域活动层下界的深度均在约17 m处,多年平衡线处冰温最低（-7.4℃）,消融区次之（-3.68℃）,积累区活动层下界冰温最高（-2.74℃）且波动最为持续,可能主要与常年积雪覆盖有关。冰温年波动随深度增加均逐渐降低,对气温变化的响应周期亦逐渐增大。与其他冰川最低温相比,老虎沟12号冰川冰温对气候变化响应敏感,过去50年来受全球变暖影响冰温显著增加。积累区深孔冰温显示50 m深度之下冰温呈线性上升,垂直增温率为0.033℃·m^-1,据此推测其底部冰温为0.02℃,主要与底部应变热有关。     

利用深地震反射剖面开展矿集区深部结构的探测:现状与实例

深地震反射剖面技术以其探测精度高的优势被作为岩石圈精细结构研究的先锋技术,并在全球典型矿集区结构探测中发挥了重要作用.为深入研究青藏高原碰撞造山成矿系统深部结构与成矿过程,本文系统总结了深地震反射技术发展现状,梳理了该技术在加拿大、澳大利亚、中国、俄罗斯、瑞典等全球多个国家的典型矿集区的应用实例,归纳总结了地壳深部结构对矿集区控矿因素的影响,阐述了地壳、上地幔深部结构与深部成矿过程的关系.从全球实例看,深地震反射剖面探测成果为大型矿集区的形成提供了深部线索,反射透明区可能是地幔流体向上运移通道,形成矿集区的成矿物质与能量来源,表明地幔物质参与了成矿作用;具有很强反射特征的断裂系统,包括大型断层、滑脱面和剪切带,是成矿流体从下地壳向上迁移的通道;矿集区深地震反射剖面中“亮点”反射可能是火山活动的深部岩浆上涌至中地壳后而形成的残余岩浆囊的反映.揭露精细的矿集区深部结构不但对矿集区构造历史演化的重建具有重要作用,还对未来成矿潜力和前景靶区的确定具有重要指导意义.     

新和地1井复杂地层水泥封孔护壁造斜技术

新和地1井在钻进1314.00～1419.98 m孔段时钻遇巨厚破碎带,地层高度破碎、大倾角、富含水系,孔壁掉块、水敏坍塌现象严重。钻进时孔内阻力大,钻具放不到底,孔内事故多发,破碎带难以钻穿。为处理孔内事故并钻穿巨厚破碎带,采用水泥封孔护壁造斜技术。受孔内复杂因素影响,特别是1358.76～1396.46 m破碎带内水系对水泥浆的稀释和冲蚀破坏作用,前期多次水泥封孔失败,浪费了大量物资及工期。现场通过试验,总结出了一套有针对性的、实用的技术方案,解决了现场的水泥封孔技术难题,提高了水泥封孔护壁造斜的成功率。新和地1井深孔复杂地层水泥封孔护壁造斜技术对今后施工类似工程具有一定的参考意义。     

日照黄海海域冷水团勘察工程施工工艺探究

日照万泽丰渔业有限公司黄海冷水团优质鱼类绿色养殖项目是山东省首批公布的新旧动能转换重大项目,规划海域面积20 km2。工程勘察是工程建设项目首先开展的基础性工作,是项目选址、设计和施工的重要依据。本文通过有效盘活有限资源,科学论证、严谨施工,创新钻探船改造、重力导向装置实现深海套管安放,成功实施了该项目的工程勘察工作,为远海深水勘察施工提供了经验。     

济南典型地层HSS参数选取及适用性研究

针对济南地区典型地层上的基坑工程,土体采用PLAXIS 3D中的硬化土小应变（HSS）模型,建立了有限元模型,并根据实际监测数据结合位移反分析技术,得到了该典型地层下土体HSS模型参数的一般选取方法。之后简化模型,分别采用土体的HSS模型与Mohr-Coulomb（M-C）模型进行有限元分析,对比基坑开挖至不同深度时,应用两种模型模拟所得挡土墙变形与墙后地表沉降的差异。结果表明：基坑数值分析中,土体采用M-C模型与HSS模型所得结果的差异随基坑挖深增加而增加,且采用HSS模型所得结果更符合深基坑的实际变形。综合考虑采用HSS模型与M-C模型建模时的参数选取难易程度、经济性以及两种模型数值分析的工程适用性,建议基坑开挖超过15 m时,土体采用HSS模型进行数值分析,反之可采用M-C模型。研究结果对指导深基坑支护设计及岩土工程参数的勘察、选取,具有重要参考价值。