The formation of the Oort cloud in open cluster environments

We study the influence of an open cluster environment on the formation and current structure of the Oort cloud. To do this, we have run 19 different simulations of the formation of the Oort cloud for 4.5 Gyrs. In each simulation, the Solar System spends its first 100 Myrs in a different open cluster environment before transitioning to its current field environment. We find that, compared to forming in the field environment, the inner Oort cloud is preferentially loaded with comets while the Sun resides in the open cluster and that most of this material remains locked in the interior of the cloud for the next 4.4 Gyrs. In addition, the outer Oort cloud trapping efficiencies we observe in our simulations are lower than previous formation models by about a factor of 2, possibly implying an even more massive early planetesimal disk. Furthermore, some of our simulations reproduce the orbits of observed extended scattered disk objects, which may serve as an observational constraint on the Sun's early environment. Depending on the particular open cluster environment, the properties of the inner Oort cloud and extended scattered disk can vary widely. On the other hand, the outer portions of the Oort cloud in each of our simulations are all similar.     

Core formation in giant gaseous protoplanets

Sedimentation rates of silicate grains in gas giant protoplanets formed by disk instability are calculated for protoplanetary masses between 1 MSaturn to 10 MJupiter. Giant protoplanets with masses of 5 MJupiter or larger are found to be too hot for grain sedimentation to form a silicate core. Smaller protoplanets are cold enough to allow grain settling and core formation. Grain sedimentation and core formation occur in the low mass protoplanets because of their slow contraction rate and low internal temperature. It is predicted that massive giant planets will not have cores, while smaller planets will have small rocky cores whose masses depend on the planetary mass, the amount of solids within the body, and the disk environment. The protoplanets are found to be too hot to allow the existence of icy grains, and therefore the cores are predicted not to contain any ices. It is suggested that the atmospheres of low mass giant planets are depleted in refractory elements compared with the atmospheres of more massive planets. These predictions provide a test of the disk instability model of gas giant planet formation. The core masses of Jupiter and Saturn were found to be ∼0.25 M_⊕ and ∼0.5 M_⊕, respectively. The core masses of Jupiter and Saturn can be substantially larger if planetesimal accretion is included. The final core mass will depend on planetesimal size, the time at which planetesimals are formed, and the size distribution of the material added to the protoplanet. Jupiter's core mass can vary from 2 to 12 M_⊕. Saturn's core mass is found to be ∼8 M_⊕.     

地下水源热泵水井泵砂与堵塞原因分析

地下水源热泵系统常会出现抽水井泵砂、抽水井和回灌井堵塞等问题,影响系统的正常运行或系统效率。以湖北省荆州市某地下水源热泵工程为例,分析了江汉平原广泛分布的卵砾石夹细砂含水层中成孔方法选择、滤料及过滤管设计中存在的问题;指出了目前在过滤管外包不锈钢丝网是防止在细砂层中水井泵砂的有效手段之一,但宜与泥浆密度轻、对地层污染小的反循环成孔工艺配合使用,且仍要根据含水层的颗粒级配曲线选择滤料,发挥滤料的过滤作用,避免过滤压力转移到包网过滤管,以减少抽水井堵塞。     

深部切顶沿空成巷关键参数研究及工程应用

传统充填沿空留巷工艺繁琐﹑留巷速度慢,与现代化高强度开采要求不相适应,由此提出了切顶沿空成巷无煤柱开采新技术,其中关键参数设计是该技术的核心问题之一,对留巷的稳定性具有较大影响。以城郊煤矿21304工作面为研究背景,采用理论分析、数值模拟和现场试验等方法,对切顶沿空成巷关键参数进行了系统研究。基于岩石碎胀自承特性和围岩结构“S-R”稳定原理,推导出切顶高度﹑切顶角度的理论计算公式;建立了聚能爆破力学模型,并结合数值模拟和现场试验,确定了聚能爆破装药量及钻孔间距。研究结果表明：合理的切顶参数能够切断巷道顶板与采空区岩层间的力学关系,使采空区顶板沿切缝顺利垮落,碎胀的矸石可有效支撑上覆顶板,限制其回转下沉,减弱覆岩运动对留巷的扰动作用,沿空巷道围岩变形量明显减小。根据理论计算﹑数值分析和现场试验研究成果,确定了城郊煤矿21304工作面切顶沿空成巷关键参数,并在现场进行了应用,回采后沿空巷道侧向顶板能够迅速切落形成巷帮,留巷稳定后各项指标均能满足现场使用要求。     

Timings of early crustal activity in southern highlands of Mars:Periods of crustal stretching and shortening

Extensional and compressional structures are globally abundant on Mars. Distribution of these structures and their ages constrain the crustal stress state and tectonic evolution of the planet. Here in this paper, we report on our investigation over the distribution of the tectonic structures and timings of the associated stress fields from the Noachis-Sabaea region. Thereafter, we hypothesize possible origins in relation to the internal/external processes through detailed morphostructural mapping. In doing so, we have extracted the absolute model ages of these linear tectonic structures using crater size-frequency distribution measurements, buffered crater counting in particular. The estimated ages indicate that the tectonic structures are younger than the mega impacts events(especially Hellas) and instead they reveal two dominant phases of interior dynamics prevailing on the southern highlands, firstly the extensional phase terminating around3.8 Ga forming grabens and then compressional phase around 3.5-3.6 Ga producing wrinkle ridges and lobate scarps. These derived absolute model ages of the grabens exhibit the age ca. 100 Ma younger than the previously documented end of the global extensional phase. The following compressional activity corresponds to the peak of global contraction period in Early Hesperian. Therefore, we conclude that the planet wide heat loss mechanism, involving crustal stretching coupled with gravitationally driven relaxation(i.e.,lithospheric mobility) resulted in the extensional structures around Late Noachian(around 3.8 Ga). Lately cooling related global contraction generated compressional stress ensuing shortening of the upper crust of the southern highlands at the Early Hesperian period(around 3.5-3.6 Ga).     

利用COSMIC掩星资料研究青藏高原地区大气边界层高度

以往关于青藏高原边界层的研究都是基于个别站点的常规观测,对青藏高原边界层的整体性认识受限。GPS掩星资料具有测量精度高和垂直分辨率高的特性,其廓线中含有大量有价值的边界层信息。利用2007—2013年COSMIC掩星资料,通过计算大气折射率最小梯度来确定边界层高度,并用无线电探空资料对结果进行了检验。在此基础上,对青藏高原地区边界层高度的特征及其形成机制展开了研究,比较了COSMIC掩星确定的边界层高度和ERA-Int的差别,讨论了最小梯度法用于边界层研究的不确定性。结果表明:青藏高原上COSMIC掩星和无线电探空数据检测的边界层高度相关系数为0.786,平均值偏差为0.049 km,均方根误差为0.363 km,COSMIC掩星数据检测的边界层高度和无线电探空的结果非常接近。青藏高原上边界层高度呈现西高东低的分布特征,高原中西部边界层高度主要为1.8—2.3 km,而高原东部边界层为1.4—1.8 km,最大值在高原西南部。青藏高原地区边界层有明显的季节差异,冬季高原上大部分地区边界层高度超过2.0 km;春季大部分地区高度降低,但在受印度季风影响的高原南部有明显的抬升,最大值可超过3.0 km;夏季高原上边界层高度开始升高,大部分地区超过1.8 km;秋季又开始回落。青藏高原以北塔克拉玛干沙漠和高原以南印度季风活动区是两个高值区,北部的沙漠地区边界层高度在夏季最高,南部印度季风活动区在季风爆发前（4月）达到全年最大值。青藏高原中西部地区有水平风辐合以及广泛的上升运动,为边界层的发展提供了动力条件,而东部的下沉运动对边界层的发展有抑制作用。青藏高原边界层各个季节的空间分布与地表感热通量分布一致。COSMIC掩星资料确定的边界层高度和ERA-Int相比,空间分布基本一致但ERA-Int边界层高度明显偏低。当有系统性强逆温存在的时候,或者云中液态水或冰水含量较大时,用最小梯度法检测的边界层高度不确定性增加。      

土−水特征曲线测量过程中孔隙分布的演化规律探讨

测量了在宽广吸力范围内原状样和压实样的脱湿持水曲线,对比分析了单双峰结构持水性能的差异;并利用压汞试验测试两种土样在脱湿过程的孔隙分布,分析了两者的差异并探讨了脱湿过程孔隙的演化规律;在考虑收缩变形的基础上,基于孔隙分布曲线确定了土?水特征曲线的基本参数。试验结果表明：原状样在宽广吸力范围内基本上呈单峰孔隙结构;饱和压实样具有单峰孔隙结构,随着吸力的增加,双峰结构越来越明显,当吸力达到很大时,演化成完全双峰孔隙结构。原状样的持水曲线为经典的S形,而压实样的持水曲线在过渡段出现了水平台阶状;低吸力段,压实样的持水曲线低于原状样,而高吸力段,两者的持水曲线基本重合。基于孔隙分布曲线确定了控制持水曲线进气值和残余值的孔径,并计算出对应的吸力值,其值更符合实际物理意义。     

西南区域持续性干旱事件的行星尺度和天气尺度扰动信号

以2009-2010年发生在中国西南地区的持续性干旱事件为例,通过干旱和大气变量的物理分解得到了一些干旱事件发生的新认识.气象干旱多为年循环的气候干季与干旱扰动的叠加所致.一次干旱扰动大约为30-50天,而一次持续性干旱事件是由几次干旱扰动组成的.大气高度场和风场中存在三种时间尺度的扰动.一种是年际行星尺度的大气扰动,与ENSO冷暖事件有关,起源于赤道并传播到中高纬度地区需要2-4年.另一种是季节内行星尺度的大气扰动,与来自赤道地区的30-50天振荡有关.此外,大气中还存在天气尺度的扰动.利用行星尺度大气扰动向赤道外传播与天气尺度扰动的叠加,区域持续性干旱事件能够找到前期预报信号.     

Improved numerical solution of Dobrovol'skaya's boundary integral equations on similarity flow for uniform symmetrical entry of wedges

Dobrovol'skaya [1] presented a similarity solution for the water entry of symmetrical wedges with constant velocity. The solution involves an integral equation that becomes increasingly harder to numerically solve as the deadrise angle decreases. Zhao and Faltinsen [2] were able to present reliable results for deadrise angles down to 4°. In this paper, Zhao and Faltinsen's results are improved and reliable results for deadrise angles down to 1° are confirmed by comparing to the asymptotic solutions at small deadrise angles and the solutions by the traditional boundary element method at relatively large deadrise angles. The present similarity solution results provide a reference solution in theoretical studies of water entry problems and in developing accurate numerical solvers for simulating strongly nonlinear wave–body interactions, which flows are governed by Laplace equation or Euler equation.