Flow patterns of lobate debris aprons and lineated valley fill north of Ismeniae Fossae, Mars: Evidence for extensive mid-latitude glaciation in the Late Amazonian

A variety of Late Amazonian landforms on Mars have been attributed to the dynamics of ice-related processes. Evidence for large-scale, mid-latitude glacial episodes existing within the last 100 million to 1 billion years on Mars has been presented from analyses of lobate debris aprons (LDA) and lineated valley fill (LVF) in the northern and southern mid-latitudes. We test the glacial hypothesis for LDA and LVF along the dichotomy boundary in the northern mid-latitudes by examining the morphological characteristics of LDA and LVF surrounding two large plateaus, proximal massifs, and the dichotomy boundary escarpment north of Ismeniae Fossae (centered at 45.3°N and 39.2°E). Lineations and flow directions within LDA and LVF were mapped using images from the Context (CTX) camera, the Thermal Emission Imaging Spectrometer (THEMIS), and the High Resolution Stereo Camera (HRSC). Flow directions were then compared to topographic contours derived from the Mars Orbiter Laser Altimeter (MOLA) to determine the down-gradient components of LDA and LVF flow. Observations indicate that flow patterns emerge from numerous alcoves within the plateau walls, are integrated over distances of up to tens of kilometers, and have down-gradient flow directions. Smaller lobes confined within alcoves and superposed on the main LDA and LVF represent a later, less extensive glacial phase. Crater size-frequency distributions of LDA and LVF suggest a minimum (youngest) age of 100 Ma. The presence of ring-mold crater morphologies is suggestive that LDA and LVF are formed of near-surface ice-rich bodies. From these observations, we interpret LDA and LVF within our study region to result from formerly active debris-covered glacial flow, consistent with similar observations in the northern mid-latitudes of Mars. Glacial flow was likely initiated from the accumulation and compaction of snow and ice on plateaus and in alcoves within the plateau walls as volatiles were mobilized to the mid-latitudes during higher obliquity excursions. Together with similar analyses elsewhere along the dichotomy boundary, these observations suggest that multiple glacial episodes occurred in the Late Amazonian and that LDA and LVF represent significant reservoirs of non-polar ice sequestered below a surface lag for hundreds of millions of years.     

Resolved spectroscopy of Mercury in the near-IR with SpeX/IRTF

We present resolved near-infrared spectra of Mercury scanning 70% of the surface in latitude and longitude from three separate observations, allowing us to perform a compositional investigation of its surface. By scanning the surface we find that all spectra in our sample are remarkably similar suggesting overall compositional homogeneity. We do, however, observe a slope difference between the spectra. These slope changes are most likely due to differences in the emission angle over different parts of the surface. We confirm the presence of a 1.1 μm feature that had been previously detected (Warell, J. et al. [2006]. Icarus 180, 281-291) and attributed to Ca-rich clinopyroxene. Finally, we investigated Mercury’s surface composition by comparing its spectrum with ground-based lunar spectra, lunar soil spectra collected in the laboratory, and analysis with a simple linear mixing model using various minerals as end-members. The result of this compositional investigation reveals that Mercury’s surface composition is likely to be quite different from the Moon’s. While low-Ca iron-rich pyroxenes are main surface components on the Moon (abundance varying from ∼5% to ∼35%), their abundance on Mercury may not exceed 5%. We also find that a Ca-rich clinopyroxene (in the hedenbergite-diopside series) is likely to be a main component of Mercury’s surface whereas this mineral is almost absent on the Moon. Our analysis also suggests the possible presence of olivine. We find that Mercury’s slope is less red than that of the Moon, in agreement with results from MESSENGER (McClintock, W.E., and 12 colleagues [2008]. Science 321, 62-65), and composition rather than variation of space weathering is likely the cause of this difference.     

Evidence for surface variegation in Rosetta OSIRIS images of asteroid 2867 Šteins

The OSIRIS camera onboard Rosetta successfully acquired images of asteroid 2867 Steins through a variety of color filters during the flyby on 5 September 2008. The best images of this 5 km diameter asteroid have a resolution of 78 m per pixel. We process the images by deconvolving with the point spread function and enlarging through the Mitchell-Netravali filter. The enhanced set is analyzed by means of various techniques (PCA, band ratios, stereo anaglyphs) to study surface morphology and search for variegation. We identify a landslide, which supports a YORP origin for Steins’ unusual diamond shape. In addition, we find that the interior of one of two large craters on the south pole is bluer than the rest of the body.     

北太平洋海表面高度(SSH) 与风应力变化的关系

利用1958-2008年的北太平洋海表面高度和风应力资料,并与ENSO和PDO指数进行相关分析.结果发现,风应力及其经向分量主要通过季节振动影响海表面高度(SSH)的年周期变化,纬向风应力主要通过多年振动影响SSH的ENSO和PDO周期.纬向风应力和SSH均以黑潮延伸体主轴为界,两侧呈现出相反的升降趋势,SSH为北降南升,纬向风应力南降北升.风应力和SSH升降趋势相同,均表现为“上升—下降—上升”的变化特征.在地形变化剧烈、等深线南北分布的海区,西风增强会导致SSH升高,且西侧升高较为明显.北风增强将导致北太平洋西岸SSH升高,东岸SSH降低.     

Occurrence and fate of polycyclic aromatic hydrocarbons in the coastal surface microlayer

Polycyclic aromatic hydrocarbons (PAHs) were measured in the coastal sea surface microlayer (SML), the sub-surface waters (SSW) and the overlying atmosphere in order to investigate the influence of the SML on contaminant enrichment and air-sea exchange. Samples were collected at two contrasting locations of the NW Mediterranean, one urban influenced (off Barcelona, Spain) and another comparatively clean (off Banyuls-sur-Mer, France). Statistical data analysis confirmed the accumulation of PAHs in the SML with respect to the SSW (20.3+/-9.1 vs. 13.1+/-10.0 ng L(-1) in the dissolved phase; 709+/-207 vs. 158+/-111 ng g(-1) in the particulate phase). This accumulation was higher at the contaminated location (Barcelona station) compared with the more pristine one, with PAH enrichments 1.5 and 4.5 times higher for the dissolved and particulate phases, respectively, indicating that the enrichment of PAHs in the SML is dominated by particle transport processes.     

玉树地震地表破裂调查与灾后重建避让选址研究

2010年4月14日07时49分40.7秒,青海省玉树县发生Ms7.1级地震。通过现场调查和分析,玉树地震的发震断裂是甘孜—玉树活动断裂的玉树段,地震产生的地表破裂长度为23km,走向北西西—北西,总体表现为左旋走滑特征,可进一步分为3段:西段呈连续延伸的左旋走滑破裂,在隆宝镇的"郭央烟宋多"附近(坐标:北纬33°03′11″、东经96°51′26″)最大水平位移达1.75m,可定为宏观震中;中段主要位于县城南侧,由多条右阶斜列的破裂组成;东段表现为逆冲兼左旋走滑。玉树地震除了造成大量房屋破坏外,次生地质灾害主要包括:地震砂土液化及其引起的公路变形、地震滑坡、地震诱发水渠破坏及其链生土质滑坡和泥石流等。通过对内外动力地质灾害的综合分析,初步提出了玉树地震灾区灾后重建避让选址的建议。     

Rapid Identification and Emergency Investigation of Surface Ruptures and Geohazards Induced by the M_s 7.1 Yushu Earthquake

<正>The rapid identification based on InSAR technology was proved to be effective in our emergency investigation of surface ruptures and geohazards induced by the Yushu earthquake.The earthquake-generating fault of the Yushu earthquake is the Yushu section of the Garze-Yushu faults zone.It strikes NWW-NW,23 km long near the Yushu County seat,dominated by left-lateral strike slip,and appearing as a surface rupture zone.The macroscopic epicenter is positioned at Guo-yang-yan -song-duo of Gyegu Town(33°03'11"N,96°51'26"E),where the co-seismic horizontal offset measured is 1.75 m.Geohazards induced by the Yushu earthquake are mainly rockfalls,landslides,debris flows, and unstable slopes.They are controlled by the earthquake-generating fault and are mostly distributed along it.There are several geohazard chains having been established,such as earthquake,canal damage,soil liquefying,landslide-debris flow,earthquake,soil liquefying,roadbed deformation,etc.In order to prevent seismic hazards,generally,where there is a visible surface rupture induced by the Yushu earthquake,reconstruction should be at least beyond 20 m,on each side,from it.Sufficient attention should also be given to potential geohazards or geohazard chains induced by the earthquake.     

堆载下单桩负摩阻力工作性状非线性数值分析

利用三维非线性数值方法对一算例在堆载作用下桩侧负摩阻力进行了计算分析。计算结果揭示了摩擦型、端承型桩负摩阻力工作性状的异同;分析了堆载速度、桩顶荷载对负摩阻力的影响:堆载越快,负摩阻力越小;在无桩顶荷载作用下,由负摩阻力引起的下拉荷载最大,可视为常规方法设计的上限值;桩顶荷载与堆载施工顺序对负摩阻力的影响也很大,先施加桩顶荷载,后进行堆载所产生的负摩阻力最大,反之最小。     

汶川地震地表破裂面形貌特征

准确描述破裂面形貌对于我们理解地震断层作用是非常重要的,破裂面的形貌特征包含许多关于地震和断层机制的有用信息。在Mw7.9 2008汶川地震中断层活动产生了两个新鲜的破裂面,八角庙破裂面和沙坝破裂面。我们使用3D便携式激光扫描仪(Tri mble GX)对两个破裂表面进行测量,在野外微观尺度上研究了破裂面形貌特征。通过能谱密度和均方值两个方法分析破裂面形貌,新鲜的破裂面表现为自相仿性,能谱密度和均方值均与剖面长度存在幂律关系。在能谱密度与空间频率的对数图中,能谱密度曲线存在明显的拐点,该拐点所对应的波长称为"特征波长",表明单一分形不能准确描述破裂面形貌。八角庙破裂面在平行滑动方向上的特征波长为7 mm,在垂直方向上特征波长略大一些(区域Ⅰ为10 mm,区域Ⅱ为9 mm);沙坝破裂面在平行滑动方向上的特征波长为8 mm,但垂直方向上特征波长略小(6 mm)。均方值曲线的最小二乘拟合直线的斜率为Hurst指数,该指数依赖于剖面线方向并描述破裂面形貌的各向异性,H指数的最小值和最大值分别与平行擦痕和垂直擦痕方向对应,这与野外断层面擦痕测量结果一致。沙坝破裂面的H指数极坐标图中存在次级H指数峰值(对应剖面线方向为85°和160°),这揭示破裂面上存在一组隐匿擦痕。该组隐匿擦痕为汶川地震之前断层活动中形成的,但这还不足以推测上一次断层活动的时间和规模。另外,通过比较新鲜节理面和破裂面表明H指数是否大于0.8反映了断层类型。在整个空间频率域上,能谱密度曲线斜率(-α)和均方值曲线斜率(H)的线性拟合关系为α=1.22+1.72H,并不严格满足两者之间理论关系式,α=1+2H。这个差异是由于测量信号噪音、破裂面的多分形性和分析方法的差异造成的。     

皖南某高速公路强风化千枚质板岩边坡变形特征及稳定性分析

以皖南地区某强烈变形的强风化千枚质板岩边坡为例,通过对其工程地质条件的调查,结合边坡岩体结构类型和结构面组合特征,对其变形破坏特征及稳定性进行了分析和评价。研究结果表明,边坡的变形受坡内软弱岩体(挤压破碎带)控制,剪应力的集中易使坡体产生圆弧形滑动,据此定量评价边坡的稳定性,提出合理的支护方案,减小地质灾害发生的可能。