A search for the 53-MHz OH line near G48.4−1.4 using the National MST Radar Facility

We present the results of a search for the ground-state hyperfine transition of the OH radical near 53 MHz using the National Mesosphere–Stratosphere–Troposphere (MST) Radar Facility at Gadanki, India. The observed position was G48.4−1.4 near the Galactic plane. The OH line is not detected. We place a 3σ upper limit for the line flux density at 39 Jy from our observations. We also did not detect recombination lines (RLs) of carbon, which were within the frequency range of our observations. The 3σ upper limit of 20 Jy obtained for the flux density of carbon RLs, along with observations at 34.5 and 327 MHz, are used to constrain the physical properties of the line-forming region. Our upper limit is consistent with the line emission expected from a partially ionized region with electron temperature, density and path lengths in the range 20–300 K, 0.03–0.3 cm⁻³ and 0.1–170 pc, respectively.     

Diffuse interstellar bands in low E (B – V) objects

We analyse spectra of slightly reddened, early-type stars in which the major diffuse interstellar bands at 5870 and 5797 Å are either strong or weak in relation to E(B – V) . It is demonstrated that among the low E(B – V) objects one can find stars obscured by 'sigma' as well as 'zeta' type clouds. The profiles of the diffuse bands seem not to be dependent on the total opacities of the interstellar clouds. We also discuss the physical conditions leading to the formation of the diffuse band carriers in low-opacity interstellar clouds; the carriers are apparently formed in media in which one can observe complex velocity fields.     

Mid-infrared imaging of WL 16: the spatial distribution of the hydrocarbon emission features

We present arcsec-resolution images at 8.2, 10.0 and 11.3 μm of the unusual young object WL 16 in Ophiuchus, which has an extended envelope of fluorescing hydrocarbon molecules. To the limit of achieved sensitivity, the faint 10.0-μm continuum has a surface-brightness distribution that is not distinguishable from those at 8.2 and 11.3 μm, where the luminosity is known to be dominated by the polycyclic aromatic hydrocarbon (PAH) emission features. We conclude that the 10-μm continuum either arises from non-equilibrium heating of small dust grains that are well mixed with the hydrocarbons or is quasi-continuous emission from the PAH particles themselves, rather than thermal equilibrium emission from macroscopic dust grains, and that there is no significant silicate absorption variation across the source. The extended hydrocarbon emission may trace a flattened, equatorial distribution of circumstellar material or arise in bipolar lobes. The former case is slightly favoured, based on currently available data, and would imply that WL 16 is a relatively evolved Herbig Ae star, the equatorial plane of which has been almost cleared of normal dust, leaving only fluorescing hydrocarbons and larger coagulated particles as a possibly transient fossil of the original circumstellar disc.     

Grain alignment in dense interstellar environments: spectropolarimetry of the 4.67-μm CO-ice feature in the field star Elias 16 (Taurus dark cloud)

We present spectropolarimetry of the solid CO feature at 4.67 μm along the line of sight to Elias 16, a field star background to the Taurus dark cloud. A clear increase in polarization is observed across the feature with the peak of polarization shifted in wavelength relative to the peak of absorption. This shows that dust grains in dense, cold environments (temperatures ∼20 K or less) can align and produce polarization by dichroic absorption. For a grain model, consisting of a core with a single mantle, the polarization feature is best modelled by a thick CO mantle, possibly including 10 per cent water-ice, with the volume ratio of mantle to bare grain of ∼5. Radiative torques could be responsible for the grain alignment provided the grain radius is at least 0.5 μm. This would require the grain cores to have a radius of at least 0.3 μm, much larger than grain sizes in the diffuse interstellar medium. Sizes of this order seem reasonable on the basis of independent evidence for grain growth by coagulation, as well as mantle formation, inside dense clouds.     

Profiles of blue and infrared diffuse interstellar bands

The paper presents a survey of profiles of reasonably strong diffuse interstellar bands (DIBs) based on the extensive set of high-resolution spectra acquired with the aid of echelle spectrographs installed at the 2-m Terskol, 2-m Pic du Midi and 1-m SAO telescopes. The surveyed diffuse interstellar bands cover the spectral ranges of blue and near-infrared, i.e the DIBs not surveyed by Krełowski & Schmidt . The possible modifications caused by stellar and telluric lines are discussed. The very broad features such as 4430 are not discussed because the shapes of their profiles, extracted from echelle spectra, are very uncertain. The signal-to-noise (S/N) ratios of the spectra are not high enough to enable discussion of the profiles of numerous weak interstellar features discovered recently.     

Closed Form Solutions of the Two-Dimensional Turning Bands Equation

The turning bands method generates realizations of isotropic Gaussian random fields by means of appropriately summed line processes. For two-dimensional simulations the relation between the isotropic correlation function of the random field and the correlation function to be simulated along the lines is given by an integral equation of Abel type. We present closed form solutions of this integral equation for almost all two-dimensional correlation models encountered in practice and discuss their numerical implementation. As an additional benefit, our tables and illustrations serve as a concise guide to correlation models useful in geostatistics.     

胶东新城金矿床控矿构造变形环境：显微构造和EBSD组构约束

新城金矿床是典型的"焦家式"破碎带蚀变岩型金矿,矿体形态和规模都严格受到断裂破碎带控制,是探讨复杂构造-流体耦合成矿系统控矿构造变形环境研究的理想选区。断裂破碎带中构造岩既是构造变形行为的载体,也是相应变形环境的受体。论文在新城金矿详细露头构造解析的基础上,系统采集该矿床控矿断裂破碎带定向构造岩样品,进行显微构造和EBSD组构分析。研究区构造岩显微构造特征主要表现为韧性变形和脆性变形。韧性变形有波状消光、带状消光、亚晶粒、动态重结晶、核幔构造、丝带构造、碎(残)斑系、扭折带、变形纹、机械双晶、蠕英结构、云母鱼等;脆性变形有书斜构造和显微裂隙等。长石(残)斑系、扭折带、变形纹、蠕英结构和石英颗粒边界迁移动态重结晶、丝带构造等矿物变形特征表明断裂带成矿前以高温韧性变形为主;石英波状消光、亚晶粒、亚颗粒旋转和膨凸动态重结晶、方解石机械双晶、长石显微裂隙充填物等矿物变形反映成矿期兼有中低温韧性变形和脆性变形;压剪性穿晶裂隙则反映出成矿后主要是低温脆性变形。根据差应力、应变测量和EBSD组构分析,将新城金矿床控矿构造变形环境可以分为3个构造期:成矿前在NW-SE向挤压作用下发生韧-脆性左行剪切变形,600~700℃,差应力61.37~111.09MPa,应变测量轴比a/c为2.295~3.978,动态重结晶石英颗粒边界分维值为1.466~1.599,反映矿区为高温中高压高应变带变形环境,应变速率较大;成矿期为NW-SE向逐渐NEE-SWW向转变的挤压作用,发生压剪性脆性变形,200~500℃,差应力65.91~135.68MPa,应变测量轴比a/c为1.403~2.204,动态重结晶石英颗粒边界分维值为1.321~1.378,反映矿区成矿期为中低温中高压低应变带变形环境,反应速率较小;成矿后在NWW-SEE向挤压作用下发生压剪变形,150~300℃,反映低温低压脆性变形环境。     

有限变形下一般流体时的热动力学模型

本文针对滑坡问题的本质,提出了非不可压流体、非理想气体前提下,在有限变形框架下牵涉到质量流动的热动力学模型,得到了不同参数空间中的特征关系;并讨论了与其它相应理论间的区别。     

水-岩化学作用对岩体变形破坏力学效应研究进展

水—岩化学作用对岩体变形破坏力学效应的研究涉及力学和化学两方面,也即为地球化学与岩体力学两个研究领域的交叉。针对水化学作用对岩体力学性质的影响机理,较系统地总结了该研究领域中的现状和研究新进展,分析了其研究方法,指出了今后的研究方向和主要研究内容,并认为此方面的研究将在工程地质学中占重要地位。     

Polygonal deformation bands

We report for the first time the occurrence of polygonal faults in sandstone, which is compelling given that layer-bound polygonal fault systems have been observed so far only in fine-grained sediments such as clay and chalk. The polygonal faults are shear deformation bands that developed under shallow burial conditions via strain hardening in dm-wide zones. The edges of the polygons are 1–5 m long. The shear deformation bands are organized as conjugate faults along each edge of the polygon and form characteristic horst-like structures. The individual deformation bands have slip magnitudes ranging from a few mm to 1.5 cm; the cumulative average slip magnitude in a zone is up to 10 cm. The deformation bands heaves, in aggregate form, accommodate a small isotropic horizontal extension (strain <0.005). The individual shear deformation bands show abutting T-junctions, veering, curving, and merging where they mechanically interact. Crosscutting relationships are rare. The interactions of the deformation bands are similar to those of mode I opening fractures. The documented fault networks have important implications for evaluating the geometry of km-scale polygonal fault systems in the subsurface, top seal integrity, as well as constraining paleo-tectonic stress regimes.