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Cost‐effective non‐metric photogrammetry from consumer‐grade sUAS: implications for direct georeferencing of structure from motion photogrammetry

The declining costs of small Unmanned Aerial Systems (sUAS), in combination with Structure‐from‐Motion (SfM) photogrammetry have triggered renewed interest in image‐based topography reconstruction. However, the potential uptake of sUAS‐based topography is limited by the need for ground control acquired with expensive survey equipment. Direct georeferencing (DG) is a workflow that obviates ground control and uses only the camera positions to georeference the SfM results. However, the absence of ground control poses significant challenges in terms of the data quality of the final geospatial outputs. Notably, it is generally accepted that ground control is required to georeference, refine the camera calibration parameters, and remove any artefacts of optical distortion from the topographic model. Here, we present an examination of DG carried out with low‐cost consumer‐grade sUAS. We begin with a study of surface deformations resulting from systematic perturbations of the radial lens distortion parameters. We then test a number of flight patterns and develop a novel error quantification method to assess the outcomes. Our perturbation analysis shows that there exists families of predictable equifinal solutions of K₁‐K₂ which minimize doming in the output model. The equifinal solutions can be expressed as K₂ = f (K₁) and they have been observed for both the DJI Inspire 1 and Phantom 3 sUAS platforms. This equifinality relationship can be used as an external reliability check of the self‐calibration and allow a DG workflow to produce topography exempt of non‐affine deformations and with random errors of 0.1% of the flying height, linear offsets below 10 m and off‐vertical tilts below 1°. Whilst not yet of survey‐grade quality, these results demonstrate that low‐cost sUAS are capable of producing reliable topography products without recourse to expensive survey equipment and we argue that direct georeferencing and low‐cost sUAS could transform survey practices in both academic and commercial disciplines. Copyright © 2016 John Wiley & Sons, Ltd.     

模糊神经网络在台风云系图象识别中的应用

利用数学形态学方法对台风云系进行区域分割，计算并统计出了台风云系纹理特征的概率密度，然后结合模糊判别技术，利用多层神经网络对ＧＭＳ云图的台风云系进行图象识别，结果表明，该方案是成功的。     

中国大陆科学钻探主孔榴辉岩类岩石退变质过程——对超高压变质地体隆升的启示

中国大陆科学钻探的实施，揭示了深俯冲陆壳的三维结构。超高压变质岩的岩相学详细观察，发现榴辉岩类岩石占0—2000米岩心的60％。大多数榴辉岩的原岩具有长期居留地壳的历史，但是分布在607～783米附近的石榴单斜辉石岩，在成因上与石榴橄榄岩关系密切。从矿物成分，岩石化学特征上看他们构成超镁铁-镁铁质的岩浆杂岩，是俯冲过程中，地幔物质加入于深俯冲的岩片并一起遭受超高压变质作用。榴辉岩质的片麻岩，部分相当于所谓的副片麻岩，在主孔也占一定的地位。实际是中酸性成分的火成岩超高压变质的产物。花岗质片麻岩有多种类型，根据其中所夹的角闪黑云片岩残留体看来大部分应属角闪黑云斜长片麻岩选择性部分熔融的产物。榴辉岩类的变质演化可分为3个阶段。第一阶段(M1约230—240Ma)是超高压变质的峰期，其证据是石榴石、绿辉石、金红石中均发现柯石英的微粒包裹物，石榴橄榄岩中的钛斜硅镁石是其超高压变质历史的见证。第二阶段(M2，226—219Ma)早期退变质阶段，超高压变质岩退变为高压榴辉岩相和角闪岩相岩石，冠状体和后成合晶的生长是此阶段的标志，这些特征性结构反应了岩石的不平衡和再平衡的历史，说明了超高压变质地体的快速隆升。后来(219～180Ma)超高压变质地体长期处于中下地壳，在流体影响下，榴辉岩质片麻岩退变成的黑云角闪斜长片麻岩及绿帘黑云(角闪)片麻岩，他们经选择性部分熔融或经超临界流体的K交代作用转变为黑云角闪二长片麻岩(即所谓正片麻岩)。其中多含有铈褐帘石，成分环带明显，La／Ce=0．42—0．72，且边沿均有绿帘石的边，代表后期叠加的绿帘钠长角闪岩相退变质。第三阶段(M3：170—180Ma)以糜棱岩和构造角砾岩的出现为特征，代表与二次隆升的脆韧性脆性变形的过渡，这些构造岩的基质普遍发育绿泥石、阳起石和方解石，说明了绿片岩相的退变质。所有上述3期的变质作用均与榴辉岩所经历的构造过程相关。显微结构分析可以揭示结晶作用和变形作用之间的相对时序。基于现今已发表的同位素年代学数据可以将苏鲁地区中生代不同阶段的变质作用与构造过程相互联系起来。CCSD主孔所见的变质演化和相关的变形事件对中国大陆中生代大陆动力学提供如下启示；可以肯定华北和杨子两个板块在三叠纪的碰撞(-240Ma)必然引起巨量地壳物质深俯冲至地幔深度，发生超高压变质。超高压变质岩的早期退变质是一个绝热隆升的过程，而后长期滞留中下地壳，发生部分熔融，接着引发进一步的隆升导致伸展体制，伴随以绿帘钠长角闪岩至绿片岩相的退变质。     

星载降水雷达机载校飞试验：地基多通道微波辐射计估算雷达路径积分衰减

介绍了在雷达观测降水试验中如何配合利用地基微波辐射计估算雷达路径积分衰减(PIA)的一种方法.所用的GPS高空探空资料和地基多通道微波辐射计的观测资料,均为中国首次星载降水雷达机载校飞试验中获得的数据.由于常规探空资料中没有云水含量的直接信息,因此,通过绝热液态水含量分析方法,从GPS探空数据中计算得到这些云参数值.用MWMOD进行亮温模拟并计算液态水含量.在晴空条件下,用该模式模拟了地基多通道微波辐射计12个通道的下行辐射亮温.通过设置相对湿度阈值,利用MWMOD模式自带的绝热液态水含量分析方法,从探空廓线中分析出液态水廓线,进而模拟出有云情况下的下行辐射亮温.辐射传输模式的模拟亮温和地基多通道微波辐射计观测亮温的对比表明,进行云分析之后的模拟亮温值更接近于实测值.由此,利用由辐射传输模式和地基微波辐射计,从探空廓线中分析出液态水廓线,计算出有云情况下的大气整层透过率,进而得到路径积分衰减,为降水雷达衰减订正提供一种有效手段.     

利用 LiDAR 点云提取有地形约束的光滑海岸线

针对传统海岸线提取算法误差大、在地形突变区域形变大的缺点,提出了一种基于离散 LiDAR 点云提取有地形约束海岸线的方法.首先,通过离散点云构建约束三角网,减少内插规则格网的误差并且保证海岸线不穿越地形结构;其次,进行顾及地形结构的点云高程修正,在数据源上缓解海岸线的平滑问题;最后采取二次多项式法消除毛刺,利用动态阈值张力样条函数内插生成光滑海岸线.     

Formation of interstellar clouds: Parker instability with phase transitions

We numerically follow the nonlinear evolution of the Parker instability in the presence of phase transitions from a warm to a cold H  i interstellar medium in two spatial dimensions. The nonlinear evolution of the system favours modes that allow the magnetic field lines to cross the galactic plane. Cold H  i clouds form with typical masses  ≃10⁵ M_⊙  , mean densities  ≃20 cm⁻³  , mean magnetic-field strengths  ≃4.3 μG  (rms field strengths  ≃6.4 μG  ), mass-to-flux ratios  ≃0.1–0.3  relative to critical, temperatures  ≃50 K  , (two-dimensional) turbulent velocity dispersions  ≃1.6 km s⁻¹  and separations  ≃500 pc  , in agreement with observations. The maximum density and magnetic-field strength are  ≃10³ cm⁻³  and  ≃20 μG  , respectively. Approximately 60 per cent of all H  i mass is in the warm neutral medium. The cold neutral medium is arranged into sheet-like structures both perpendicular and parallel to the galactic plane, but it is also found almost everywhere in the galactic plane, with the density being highest in valleys of the magnetic field lines. 'Cloudlets' also form whose physical properties are in quantitative agreement with those observed for such objects by Heiles. The nonlinear phase of the evolution takes ≲30 Myr, so that, if the instability is triggered by a nonlinear perturbation such as a spiral density shock wave, interstellar clouds can form within a time suggested by observations.     

Inefficient star formation: the combined effects of magnetic fields and radiative feedback

We investigate the effects of magnetic fields and radiative protostellar feedback on the star formation process using self-gravitating radiation magnetohydrodynamical calculations. We present results from a series of calculations of the collapse of  50 M_⊙  molecular clouds with various magnetic field strengths and with and without radiative transfer. We find that both magnetic fields and radiation have a dramatic impact on star formation, though the two effects are in many ways complementary. Magnetic fields primarily provide support on large scales to low-density gas, whereas radiation is found to strongly suppress small-scale fragmentation by increasing the temperature in the high-density material near the protostars. With strong magnetic fields and radiative feedback, the net result is an inefficient star formation process with a star formation rate of  ≲10  per cent per free-fall time that approaches the observed rate, although we have only been able to follow the calculations for 1/3 of a free-fall time beyond the onset of star formation.     

A new, efficient stellar evolution code for calculating complete evolutionary tracks

We present a new stellar evolution code and a set of results, demonstrating its capability at calculating full evolutionary tracks for a wide range of masses and metallicities. The code is fast and efficient, and is capable of following through all evolutionary phases, without interruption or human intervention. It is meant to be used also in the context of modelling the evolution of dense stellar systems, for performing live calculations for both normal star models and merger products.
The code is based on a fully implicit, adaptive-grid numerical scheme that solves simultaneously for structure, mesh and chemical composition. Full details are given for the treatment of convection, equation of state, opacity, nuclear reactions and mass loss.
Results of evolutionary calculations are shown for a solar model that matches the characteristics of the present sun to an accuracy of better than 1 per cent; a  1 M_⊙  model for a wide range of metallicities; a series of models of stellar Populations I and II, for the mass range 0.25 to  64 M_⊙  , followed from pre-main-sequence to a cool white dwarf or core collapse. An initial–final mass relationship is derived and compared with previous studies. Finally, we briefly address the evolution of non-canonical configurations, merger products of low-mass main-sequence parents.