Model prediction capacity of ephemeral gully evolution in conservation tillage systems

Ephemeral gully (EG) erosion has an important impact on agricultural soil losses and increases field surface hydrology connectivity and transport of pollutants to nearby water bodies. Watershed models including an EG component are scarce and not yet properly evaluated. The objective of this study is to evaluate the capacity of one such tool, AnnAGNPS, to simulate the evolution of two EG formed in a conservation tillage system. The dataset for model testing included runoff measurements and EG morphological characteristics during 3 years. Model evaluation focused on EG evolution of volume, width, and length model outputs, and included calibration and testing phases and a global sensitivity analysis (GSA). While the model did not fully reproduce width and length, the model efficiency to simulate EG volume was satisfactory for both calibration and testing phases, supporting the watershed management objectives of the model. GSA revealed that the most sensitive factors were EG depth, critical shear stress, headcut detachment exponent coefficient b, and headcut detachment leading coefficient a. For EG outputs the model was additive, showing low sensitivity to interactions between the inputs. Prediction of EG spatial evolution on conservation tillage systems requires improved development of gully erosion components, since many of the processes were developed originally for traditional tillage practices or larger channel systems. Our results identify the need for future research when EG form within conservation tillage systems, in particular to study gully headcut, soil erodibility, and width functions specific to these practices.     

Solid phase characterization and metal deportment in a mussel shell bioreactor for the treatment of AMD,Stockton Coal Mine,New Zealand

The Stockton Coal Mine, located on the West Coast of New Zealand, is evaluating the use of a mussel shell bioreactor (MSB) to treat acidic metalliferous runoff from acid forming overburden. This novel approach is similar in concept to vertical flow wetlands (VFWs) and successive alkalinity producing systems (SAPS). The MSB system is a trapezoidal pit 2 m deep, 35 m long, 3–10 m wide with 60° angle sides. During operation it contained 160 tonnes (240 m³) of mussel shell material and was saturated with a 100–200 mm water cap. Influent flowed through the reactor at a mean rate of 0.3 L s⁻¹ resulting in a hydraulic retention time (HRT) of ≈6 days. The prototype MSB was in operation for a total of 1027 days, from June 2009 through March 2012, and effectively sequestered 99.7% of Al, 99.3% of Fe, 98.8% of Ni, 98.4% Tl and 99.3% of Zn, as determined from a previous evaluation of MSB performance. The MSB also effectively neutralized acidity, which resulted in an increase in influent pH from 2.8 to 6.9 in the effluent. Based on an examination of several excavated pits, five distinct reaction zones developed within the MSB. The reaction zones consisted of an allochthonous sediment layer (0–330 mm), an oxidized iron-rich ocherous layer (at 330–350 mm depth), an aluminum layer (at 350–600 mm depth) with geochemical variations throughout (350–500 mm and 500–600 mm); and a chemically reduced bottom shell layer (at 600–1100 mm). Representative samples were collected from each layer and analyzed using a combination of geochemical and physical methods to assess the stability of the secondary minerals and trace metal deportment within the MSB. Major elements Fe, Al, Ni, Tl, and Zn where preferentially associated with particular layers within the MSB. Elevated concentrations of Fe (110,000 mg kg⁻¹) were observed in the allochthonous sediment and ocherous precipitate layers, while Al (27,816 mg kg⁻¹), Ni (55 mg kg⁻¹), and Zn (655 mg kg⁻¹) were elevated within the aluminum and lower reduced depths within the MSB. Trace Tl (21 mg kg⁻¹) showed varying concentrations throughout the MSB, but was strongly correlated to lower layers of the system. Microbial biofilms were observed within the reduced portions of the shell layers often proximal to bacterial shaped sulfides. The geochemical assessment of the MSB presented in this study is the first of its kind for a MSB, and supports the argument that this system is another viable option for passive treatment of AMD.     

新疆国土资源环境信息系统设计与实现

对新疆国土资源环境信息系统的设计与实现进行了详细介绍,对系统研建中的关键技术进行了研究和探讨,提出了解决方案。系统的建成实现了利用GIS技术对国土资源环境信息的统一管理和快速检索、更新、分析与处理,填补了新疆国土资源环境遥感综合调查信息应用GIS技术综合管理应用的空白。     

GIS专业本科教学探讨--北京大学教学实例

随着社会对于地理信息系统专业人才的需求,在全世界范围内地理信息科学的教学和培训工作得到了越来越广泛的重视．作为较早开始设立地理信息系统专业的综合性大学——北京大学,在地理信息科学教学实践中积累了丰富的经验,并形成了自己的特色：重视基础,淡化专业;重视地学基础课程的学习和应用;注重理论和实践的结合,向工科倾斜;及时反映GIS的最新进展。     

区域生态功能建设规划的原理与模拟探析

在剖析区域演化历程中的生态功能变迁与导引的生态环境滞胀及危害基础上,着重利用系统生态学的原理和方法,探讨了可持续发展要求下的区域生态功能建设规划的目标、原理和研究的内容、方法及过程;提出了以产业结构、土地利用结构和空间格局调整为核心,制定区域生态功能建设规划的总体思路;创造性地将水土流失、污染物排放、社会经济发展、劳动力吸纳、人口容载和土地资源合理配置及城镇发展等模型融于一体,构建了案例区十堰市的生态环境功能综合调控模型,并借助DYNAMO语言,模拟得到了十堰市未来生态功能建设的优化方案。     

用相关分析法约简MCSs空间数据库

长江流域出现致洪大暴雨与青藏高原上中尺度对流系统(MCSs)的东移密切相关。为了寻找MCSs移动和传播的规律,我们将MCSs的移动路径与其中心附近一定范围内的环境物理量场之间建立联系,构造出MCSs东移空间数据挖掘数据库。在这个数据库中,包含由9个环境物理量生成的18个属性项,除此,还包括由MCSs本身的空间特征量构成的5个属性项,即TBB强度、面积、地理位置、形状等,共计23个属性项。利用1998年6月至8月日本地球静止气象卫星(GMS)的青藏高原逐时红外遥感云图计算出的云顶黑体辐射温度(TBB)及青藏高原高分辨率有限区域数值分析预报值系统(HLAFS)环境场物理量数据,构造出上述空间数据挖掘数据库,运用空间相关分析技术对其进行约简,结果表明：在高度(H)、温度（T）、涡度(VOR)、散度(DIV)、水汽通量散度(IFVQ)、垂直速度(W）、假相当位温（θse)、K指数(K)、相对湿度(RH)等9个因素中,高度、涡度、散度、水汽通量散度、垂直速度及k指数6个因素相对独立;而温度(T)、假相当位温(θse)、相对湿度（RH)之间相关性较强,而且与高度等其它6个因素密切相关。根据数据库约简原则,可将温度（T）、假相当位温(θse)、相对湿度(RH)3个因素生成的6个属性项从数据库中删除,以便提高数据挖掘效率。     

Detecting protoplanets with ALMA

Theoretical investigations show that planet-disk interactions cause structures in circumstellar disks, which are usually much larger in size than the planet itself and thus more easily detectable. The specific result of planet-disk interactions depends on the evolutionary stage of the disk. Exemplary signatures of planets embedded in disks are gaps and spiral density waves in the case of young, gas-rich protoplanetary disks and characteristic asymmetric density patterns in debris disks. Numerical simulations convincingly demonstrate that high-resolution imaging performed with observational facilities which are already available or will become available in the near future will allow to trace these “fingerprints” of planets in protoplanetary and debris disks. These observations will provide a deep insight into specific phases of the formation and early evolution of planets in circumstellar disks. In this context, the Atacama Large Millimeter Array (ALMA) will play a crucial role by allowing to trace features in disks which are indicative for various stages of the formation and early evolution of planets in circumstellar disks.     

Observable consequences of planet formation models in systems with close-in terrestrial planets

To date, two planetary systems have been discovered with close-in, terrestrial-mass planets     . Many more such discoveries are anticipated in the coming years with radial velocity and transit searches. Here we investigate the different mechanisms that could form 'hot Earths' and their observable predictions. Models include: (1) in situ accretion; (2) formation at larger orbital distance followed by inward 'type 1' migration; (3) formation from material being 'shepherded' inward by a migrating gas giant planet; (4) formation from material being shepherded by moving secular resonances during dispersal of the protoplanetary disc; (5) tidal circularization of eccentric terrestrial planets with close-in perihelion distances and (6) photoevaporative mass-loss of a close-in giant planet. Models 1–4 have been validated in previous work. We show that tidal circularization can form hot Earths, but only for relatively massive planets     with very close-in perihelion distances (≲0.025 au), and even then the net inward movement in orbital distance is at most only 0.1–0.15 au. For planets of less than     , photoevaporation can remove the planet's envelope and leave behind the solid core on a Gyr time-scale, but only for planets inside 0.025–0.05 au. Using two quantities that are observable by current and upcoming missions, we show that these models each produce unique signatures, and can be observationally distinguished. These observables are the planetary system architecture (detectable with radial velocities, transits and transit timing) and the bulk composition of transiting close-in terrestrial planets (measured by transits via the planet's radius).     

A Spitzer survey of young stellar objects in the Rosette Molecular Cloud

We present results from a survey of the Rosette Molecular Cloud (RMC) using both the Infrared Array Camera (IRAC) and Multiband Imaging Photometer for Spitzer (MIPS) onboard the Spitzer Space Telescope . We have mapped a region of active star formation covering an area approximately 1° by 1.5° including several previously known clusters. Spectral energy distributions (SEDs) fitted to our data combined with that from Two Micron All Sky Survey (2MASS) are used to identify young stellar objects (YSOs) with infrared (IR) excesses. We find that roughly 50 per cent of the sources are forming in clustered environments and identify seven clusters of IR excess sources including four that were previously unknown. We investigate evidence for triggering of star formation due to the ionization front, identified in Brackett-α emission, associated with the young open cluster NGC 2244. Although the position of several of the clusters of IR excess sources are coincident with the ionization front, the bulk of the youngest YSOs are located far from the ionization front, in clusters located along the mid-plane of the cloud. We conclude that although triggering from the H  ii nebula is a possible origin for some of the recent star formation, the majority of the active star formation is occurring in already dense regions of the cloud not compressed by the expansion of the H  ii region.     

Eccentricity growth of planetesimals in a self-gravitating protoplanetary disc

We investigate the orbital evolution of planetesimals in a self-gravitating circumstellar disc in the size regime (∼1–5000 km) where the planetesimals behave approximately as test particles in the disc's non-axisymmetric potential. We find that the particles respond to the stochastic, regenerative spiral features in the disc by executing large random excursions (up to a factor of 2 in radius in ∼1000 yr), although typical random orbital velocities are of the order of one tenth of the Keplerian speed. The limited time frame and small number of planetesimals modelled do not permit us to discern any net direction of planetesimal migration. Our main conclusion is that the high eccentricities (∼0.1) induced by interaction with spiral features in the disc is likely to be highly unfavourable to the collisional growth of planetesimals in this size range while the disc is in the self-gravitating regime. Thus if , as recently argued by Rice et al., the production of planetesimals gets under way when the disc is in the self-gravitating regime (either at smaller planetesimal size scales, where gas drag is important, or via gravitational fragmentation of the solid component), the planetesimals thus produced would not be able to grow collisionally until the disc ceases to be self-gravitating. It is unclear, however, given the large amplitude excursions undergone by planetesimals in the self-gravitating disc, whether they would be retained in the disc throughout this period, or whether they would instead be lost to the central star.