In situ thermal conductivity measurements of Titan's lower atmosphere

Thermal conductivity measurements, presented in this paper (Fig. 3), were made during the descent of the Huygens probe through the atmosphere of Titan below the altitude of 30 km. The measurements are broadly consistent with reference values derived from the composition, pressure and temperature profiles of the atmosphere; except in narrow altitude regions around 19 km and 11 km, where the measured thermal conductivity is lower than the reference by 1% and 2%, respectively. Only single data point exists at each of the two altitudes mentioned above; if true however, the result supports the case for existence for molecules heavier than nitrogen in these regions (such as: ethane, other primordial noble gases, carbon dioxide, and other hydrocarbon derivatives). The increasing thermal conductivity observed below 7 km altitude could be due to some liquid deposition during the descent; either due to condensation and/or due to passing through layers of fog/cloud containing liquid nitrogen-methane. Thermal conductivity measurements do not allow conclusions to be drawn about how such liquid may have entered the sensor, but an estimate of the cumulative liquid content encountered in the last 7 km is 0.6% by volume of the Titan's atmosphere sampled during descent.     

A method for averaging the perturbing function in Hill’s problem

A modified method for averaging the perturbing function in Hill’s problem is suggested. The averaging is performed in the revolution period of the satellite over the mean anomaly of its motion with a full allowance for a variation in the position of the perturbing body. At its fixed position, the semimajor axis of the satellite orbit during the revolution of the satellite is constant in view of the evolution equations, while the remaining orbital elements undergo secular and long-period perturbations. Therefore, when the motion of the perturbing body is taken into account, the semimajor axis of the satellite orbit undergoes the strongest perturbations. The suggested approach generalizes the averaging method in which only the linear (in time) term is included in the perturbing function. This method requires no expansion in powers of time. The described method is illustrated by calculating the perturbations of the semimajor axes for two distant satellites of Saturn, S/2000 S 1 and S/2000 S5. An approximate analytic solution is compared with the results of numerical integration of the averaged system of equations of motion for these satellites.     

Residual slip of sliding blocks induced by near‐fault ground motions

The response of a rigid block supported on a horizontally moving foundation through a dry‐friction contact is investigated to near‐fault ground motions. Such motions can be thought of as consisting of a coherent component (‘pulse’) and an incoherent component, which can be described as a band‐limited ‘random noise’. The equation of motion of this strongly nonlinear system is reduced to a normalized form that reveals important parameters of the problem such as the critical acceleration ratio. The response of the sliding block to a set of uniformly processed near‐fault motions, covering a sufficiently wide range of magnitudes, is evaluated numerically for selected discrete values of the acceleration ratio. For each value of the critical acceleration ratio, the numerically computed residual slips are fitted with a Weibull (Gumbel type III) extreme value probability distribution. This allows the establishment of regression equations that describe accurately design sliding curves corresponding to various levels of non‐exceedance probability. The analysis reveals that the coherent component of motion contributes significantly to the response of the sliding block. Furthermore, the relevant acceleration in specifying the critical acceleration ratio is the (normalized) amplitude, α_{H_pulse}, of the pulse and not the (normalized) amplitude of the incoherent component α_H. Finally, the incoherent component is described quantitatively in terms of the root‐mean‐square acceleration a_RMS, and an attempt is made to understand its influence on the response of the sliding block. Copyright © 2016 John Wiley & Sons, Ltd.     

地壳运动整体观论纲

本文在全面讨论了构造体系与全球运动场、板块构造与旋转扩张、断块构造、镶嵌构造、地洼说与地球自转、构造迁移的方向性及地球水圈、气圈和生物圈的运动规律以后,提出了地球动力系统统一观,并进一步论述了包括重力、热力、离心惯性力等在内的地球动力系统中,地球自转和自转速度不均衡乃是发动地壳运动的主因,而地球整体的运动和变化,又受着天体活动的影响。
本文纲要性地指出,地壳上各种地质现象与相关的自然现象是一个有联系的整体,受控于地球整体的运动系统。      

旅游空间相互作用的引力模型及其应用

客源地与目的地之间的旅游空间相互作用是必然而持久地,这深刻地影响着旅游者行为和旅游业进步,需要发展适宜的引力模型对其进行刻画和量度.长期以来,旅游引力模型在对空间阻尼的处理上类比牛顿型的幂函数衰减模式,难以克服一些固有缺陷,因此重新回到威尔逊型的指数函数衰减模式就成为一种可能选择.本文即是基于威尔逊形式,将目的地“吸引力”、客源地“出游力”和两地间的“空间阻尼”作为3 个基本解释变量类型,构建了一个基础的旅游引力模型,并重点在参数估计和模型应用上进行了初步探索.由于难以从整体上对模型的两个核心参数进行回归估计,本文首先从局部对收入弹性系数α进行回归估计,然后通过“口粒子模式法”和“出游量积分法”的引入和交互验证来确定空间阻尼系数β的合理取值.研究表明,就全国平均而言,在21 世纪初收入弹性系数可取0.64,而空间阻尼系数可取0.00322,且在空间阻尼影响下,中国大陆居民国内旅游的理论出游半径均值约为300 km.最后,本文从目的地供给视角计算了中国大陆分省区的旅游吸引力,从客源地需求视角计算了成都市到访游客的分省预期市场份额,这两个案例研究在取得一些有益发现的同时也表明威尔逊型旅游引力模型具有积极的应用潜力,值得进一步探索.     

南北两极海冰的涛动关系

本文将南极海冰分为４个区：ＳＰＩ１（０°－１２０°Ｅ），东南极海冰；ＳＰＩ２（１２０°Ｅ－１２０°Ｗ），以罗斯海为主体的海冰区；ＳＰＩ３（１２０°Ｗ－０°），以威德尔海为主体的海冰区；ＳＰＩ４，全南极海冰区。北极海冰区分为３个区：ＮＰＩ１（９０°Ｅ－１８０°－９０°Ｗ），太平洋侧冰区；ＮＰＩ２（９０°Ｗ－０°－９０°Ｅ），大西洋侧冰区；ＮＰＩ３，全北极冰区。本文使用了ＷＤＣ－Ａ的ＳＩＧＲＩＤ海冰资料，以分析南极和北极各冰区之间的相互关系。发现两极各冰区之间存在着非常复杂的相互作用。其中最突出的特征是：两极海冰之间相互作用的振源是ＮＰＩ２。ＳＰＩ３是影响南极海冰的正反馈中心。ＳＰＩ２则是南北两极海冰的负反馈中心。ＮＰＩ２，ＳＰＩ３和ＳＰＩ２之间的相互作用最强，形成涛动关系。这种涛动关系不是同时期的，而是有较长的滞后时间差。两极海冰形成周期变化，其周期为５－６年，正与ＮＰＩ２和ＳＰＩ３自身变化周期一致。另外还有更长的循环周期９－１１年     

南极中山站与北京地磁中心台1991年3月24日磁暴的变化特征

本文分析了１９９１年３月２４日急始型磁暴的变化特征。分析表明，南极极隙区与中低纬区磁暴形态差异很大。中山站地磁台的磁暴急始为ＳＣ＊型，无明显磁暴主相，它是由一组强烈的磁亚暴所组成。北京地磁中心台的磁暴急始为ＳＣ型，磁暴主相持续时间较短，变化较大。这次磁暴是由磁暴前太阳黑子相对数增多、３月２２日２２ｈ４６ｍＵＴ有３ｂ级耀斑爆发等一系列太阳活动所引起的     

Removal of Titan's noble gases by their trapping in its haze

Titan's haze, formed by photolysis of C₂H₂, C₂H₄ and HCN, was found experimentally to trap Ar, Kr and Xe with efficiencies of 3.5 × 10⁻⁴, 1.9 × 10⁻³ and 6.5 × 10⁻² [noble gas atom]/[carbon atom] in the polymer, respectively. The rate of aerosol formation and settling down of 3 × 10⁻¹³ kg m⁻² s⁻¹, as inferred from our experiments on CH₄ photolysis in the far UV [Podolak, M., Bar-Nun, A., 1979. Icarus 39, 272-276], is sufficient to reduce the mixing ratios of ³⁶Ar and ⁴⁰Ar to their low values of (2.8 ± 0.3) × 10⁻⁷ and (4.3 ± 0.1) × 10⁻³, respectively, and those of Kr and Xe to below the detection limit of 10⁻⁸.     

利用噪声记录估计福建地区中上地壳体波速度结构

In this paper,the dispersion curves of the Rayleigh wave and Love wave were extracted from the seismic noise records of 25 broadband stations of the Fujian Seismic Network, and inverted for the lithosphere velocity structure. Furthermore,the velocity model was verified by the seismic explosion observations. Our results indicate that the resolution of the lithosphere velocity structure obtained by this method is good in the shallow part,but in the deep part,inversion accuracy for the wave velocity structure is low,which is caused mainly by the small inter-station distance chosen in the paper. Thus the wave dispersion curves have high accuracy in the short-period part,but the warp of the wave dispersion curve in long-period part is large. Considering the results from both the noise inversion and the traditional inversion,we finally present a new velocity model,and the theoretical travel time calculated with the new model matches the explosion travel time very well.     

近50a来桂林市灰霾天气的气候特征及热岛效应影响

根据桂林基准站1957～2006年的观测资料,对桂林市灰霾天气的年、季变化规律及与热岛效应的关系进行了分析。结果表明,桂林市年灰霾日数平均值为30d,80年代前年灰霾日数变化相对平稳,年平均值为8.6d,处于较低水平,80年代后灰霾日数年平均值为49d,比80年代前增加了40.4d,年平均灰霾日数呈明显的线性增长趋势;灰霾日数的月季变化表现为秋冬季多,春夏季少的分布特征,秋冬两个季节的灰霾日数占全年的76%;90年代后桂林出现热岛效应,第四季度尤为明显,与灰霾天气也大多出现在这个季节的分析结果一致。