场地土层模型参数的地震动记录反演方法

考虑场地土层不同物理参数的综合反演,改进了水平与竖向谱比（Horizontal-to-Vertical Spectral Ratio,简称HVSR）混合全局优化反演方法,进一步通过土层的S、P波波速、厚度、泊松比、密度和S、P波品质因子等土层参数反演的敏感性分析,形成了可同时反演场地土层厚度及剪切波速的混合全局优化反演方法.以美国GVDA和日本IWTH27竖向强震动观测台阵为例,分别以理论HVSR及加速度观测记录获得的HVSR曲线为目标,反演获得了场地浅层速度结构,并与观测台阵场地钻孔揭示的土层模型进行比较,验证了发展的反演方法的合理性和适用性.本文研究表明,基于地震加速度记录的HVSR全局优化反演方法是获取场地土层速度结构的一种有效的途径.

     

等离子体湍动对准垂直激波中粒子加速的影响

本文利用试验粒子方法研究了在考虑等离子体湍动的情况下带电粒子在准垂直激波中的加速, 在计算中, 我们采用组合模型来拟合等离子体湍动. 计算结果表明, 在存在等离子体湍动的情况下, 粒子可横越背景磁场运动, 从而被激波反射的上游粒子在到达下游后可被等离子体湍动散射回到上游, 并再次被激波反射并加速, 这样的过程可重复很多次, 因而粒子可被加速到很高的能量. 我们还研究了激波角, 粒子的初始能量和等离子体湍动的强度, 以及相干长度和两种湍动组分强度比与加速粒子的能谱之间的关系.     

Particle acceleration and transport in the inner heliosphere

In the solar system, our Sun is Nature’s most efficient particle accelerator. In large solar flares and fast coronal mass ejections (CMEs), protons and heavy ions can be accelerated to over ~GeV/nucleon. Large flares and fast CMEs often occur together. However there are clues that different acceleration mechanisms exist in these two processes. In solar flares, particles are accelerated at magnetic reconnection sites and stochastic acceleration likely dominates. In comparison, at CME-driven shocks, diffusive shock acceleration dominates. Besides solar flares and CMEs, which are transient events, acceleration of particles has also been observed in other places in the solar system, including the solar wind termination shock, planetary bow shocks, and shocks bounding the Corotation Interaction Regions (CIRs). Understanding how particles are accelerated in these places has been a central topic of space physics. However, because observations of energetic particles are often made at spacecraft near the Earth, propagation of energetic particles in the solar wind smears out many distinct features of the acceleration process. The propagation of a charged particle in the solar wind closely relates to the turbulent electric field and magnetic field of the solar wind through particle-wave interaction. A correct interpretation of the observations therefore requires a thorough understanding of the solar wind turbulence. Conversely, one can deduce properties of the solar wind turbulence from energetic particle observations. In this article I briefly review some of the current state of knowledge of particle acceleration and transport in the inner heliosphere and discuss a few topics which may bear the key features to further understand the problem of particle acceleration and transport.     

Selection between the generalized Pareto and kappa distributions in peaks-over-threshold hydrological frequency modelling

Hydrologists use the generalized Pareto (GP) distribution in peaks-over-threshold (POT) modelling of extremes. A model with similar uses is the two-parameter kappa (KAP) distribution. KAP has had fewer hydrological applications than GP, but some studies have shown it to merit wider use. The problem of choosing between GP and KAP arises quite often in frequency analyses. This study, by comparing some discrimination methods between these two models, aims to show which method(s) is (are) recommended. Three specific methods are considered: one uses the Anderson-Darling goodness-of-fit (GoF) statistic, another uses the ratio of maximized likelihood (closely related to the Akaike information criterion and the Bayesian information criterion), and the third employs a normality transformation followed by application of the Shapiro-Wilk statistic. We show this last method to be the most recommendable, due to its advantages with sizes typically encountered in hydrology. We apply the simulation results to some flood POT datasets.

EDITOR D. Koutsoyiannis; ASSOCIATE EDITOR E. Volpi     

Field-aligned conductance values estimated from Maxwellian and kappa distributions in quiet and disturbed events using Freja electron data

We study the question of what difference it makes for the derived field-aligned conductance (K) values if one uses Maxwellian or kappa distributions for the fitting of low-orbiting satellite electron flux spectra in the auroral region. This question has arisen because sometimes a high-energy tail is seen in the spectra. In principle, the kappa fits should always be better, because the kappa distribution is a generalization of the Maxwellian. However, the physical meaning of the parameters appearing in the Maxwellian is clearer. It therefore makes sense to study under which circumstances it is appropriate to use a Maxwellian. We use Freja electron data (TESP and MATE) from two events. One of the events represents quiet magnetospheric conditions (stable arc) and the other represents disturbed conditions (surge). In these Freja events, at least, using kappa rather than Maxwellian fitting gives a better fit to the observed distribution, but the difference in K values is not large (usually less than 20%). The difference can be of either sign. However, sometimes even the kappa distribution does not provide a good fit, and one needs a more complicated distribution such as two Maxwellians. We investigate the relative contributions of the two Maxwellians to the total field-aligned conductance value in these cases. We find that the contribution of the high-energy population is insignificant (usually much less than 20%). This is because K is proportional to n/E_c E_c, where n is the source plasma density and E_c is the characteristic energy.     

MELIMEX,an experimental heavy metal pollution study: Particle size distributions in limno-corrals

The particle size distributions in three limno-corrals, located in Baldeggersee, Switzerland, have been determined by means of a Zeiss Micro-Videomat image analyzer as a function of depth and time. The distributions were measured biweekly over a period of 1 year at depths of 0 m, 2.5 m, 5 m, 7.5 m and 10 m (=above bottom). Two of the limno-corrals were charged with heavy metals, whereas the third was uncharged and served as a reference. The shape of the distributions as well as the particle concentrations in the uncharged container did not differ from the ones in the charged limno-corrals. The distributions were found to be self-preserving and independent on heavy metal load, time, depth and particle concentrations. As an average, the dependence of the distributions on the particle diameter was found to be ?1.5 to ?2.5.     

CHAMP卫星主磁场长期变化和长期加速度的分布特征

本文利用CHAMP卫星磁测资料建立的新一代地磁场模型POMME-4.2S,分析了全球和中国地区地磁长期变化X、Y、Z、H、F、J、D 7个分量以及长期加速度X、Y、Z3个分量的分布特征,比较了POMME-4.2S长期变化模型与中国长期变模型CGRF-SV的磁异常分布差异.主要结果表明,地磁长期变化磁四极子起主要贡献,长期加速度变化磁八极子贡献最大.2004.0年全球长期变化的减小要比增加大得多,地磁场总体在减弱.长期加速度在中低纬度地区变化较大,高纬度地区变化小.Z和Y分量磁异常沿经度方向正、负交错形成几个大片区,X分量主要正负磁异常成对分布于赤道两侧.长期加速度X、Y、Z3个分量的磁异常分布存在明显的关系:在Z异常焦点的南北两边出现X的异常焦点,东西两边出现Y的异常焦点.中国地区的长期变化和长期加速度变化量小,分布相对均匀.     

Particle swarm optimization of TMD by non‐stationary base excitation during earthquake

There are many traditional methods to find the optimum parameters of a tuned mass damper (TMD) subject to stationary base excitations. It is very difficult to obtain the optimum parameters of a TMD subject to non‐stationary base excitations using these traditional optimization techniques. In this paper, by applying particle swarm optimization (PSO) algorithm as a novel evolutionary algorithm, the optimum parameters including the optimum mass ratio, damper damping and tuning frequency of the TMD system attached to a viscously damped single‐degree‐of‐freedom main system subject to non‐stationary excitation can be obtained when taking either the displacement or the acceleration mean square response, as well as their combination, as the cost function. For simplicity of presentation, the non‐stationary excitation is modeled by an evolutionary stationary process in the paper. By means of three numerical examples for different types of non‐stationary ground acceleration models, the results indicate that PSO can be used to find the optimum mass ratio, damper damping and tuning frequency of the non‐stationary TMD system, and it is quite easy to be programmed for practical engineering applications. Copyright © 2008 John Wiley & Sons, Ltd.     

Electromagnetic effects during the formation of midlatitude sporadic layers

The possibility of the occurrence of sporadic layers in the ionospheric dynamo region due to the formation of thin layers with large plasma pressure gradients balancing the Ampere force is considered. Observational data confirming the validity of such an approach are presented.     

Particle path length distributions in meandering gravel‐bed streams: results from physical models

In gravel‐bed rivers with well‐de?ned pool–bar morphology, the path length of transported bed particles must be, at least during ‘channel‐forming’ ?ows, equal to the length scale of the morphology. This is the basis for some methods for estimating bed material transport rates. However, previous data, especially from ?eld tests, are often strongly positively skewed with mean much shorter than the pool–bar spacing. One possible explanation is that positively skewed distributions occur only in channels lacking distinct pool–bar topography or only at lower discharges in pool–bar channels. A series of ?ume experiments using ?uorescent tracers was used to measure path length distributions in low‐sinuosity meandering channels to assess the relation with channel morphology and ?ow conditions. At channel‐forming ?ows, 55 to 75 per cent of the tracer grains were deposited on the ?rst point bar downstream of the point of tracer input, with 15 per cent passing beyond the ?rst bar. Path length distributions are symmetrical with mean equal to the pool–bar spacing and can be described with a Cauchy distribution. In some cases there was a secondary mode close to the point of tracer introduction; this bimodal distribution ?ts a combined gamma–Cauchy distribution. Only when discharge was reduced below the channel‐forming ?ow were frequency distributions unimodal and positively skewed with no relation to the pool–bar spacing. Thus, path length distributions become more symmetrical, and mean path length increases to coincide with pool–bar spacing, as ?ow approaches channel‐forming conditions. This is a substantial modi?cation of existing models of particle transfer in gravel‐bed rivers. Copyright © 2003 John Wiley & Sons, Ltd.     

Two-dimensional simulations of katabatic layers observed during the GIMEX experiment

The hydrostatic model SALSA is used to simulate a particular event observed during the Greenland Ice Margin EXperiment “GIMEX” (on July 12th, 1991). The time evolution of the large-scale flow was incorporated in the model through time dependent boundary conditions which were updated using the closest upwind sounding. A turbulent scheme for the stable boundary layer and an appropriate parametrization of the surface fluxes implemented in the same model, are used for this study. The simulation results are discussed and compared to the available observations. The computed turbulent fluxes are correctly estimated. The model predicts a mixing zone of about 1500 m high which is in good agreement with tundra site observations. Over the ice cap, the katabatic layer is correctly simulated by the model. Its height of 80–300 m is well estimated. The comparison between the simulation and observations taken at ice cap sites is reasonably valid. The ablation computed along the ice cap corresponds well to the values reconstructed of observations at sites 4 and 9. Finally, a sensibility study to a specified westward geostrophic wind (2 ms⁻¹) shows that the consideration of this latter improves the simulated tundra wind evolution.     

The current-voltage relationship revisited: exact and approximate formulas with almost general validity for hot magnetospheric electrons for bi-Maxwellian and kappa distributions

We derive the current-voltage relationship in the auroral region taking into account magnetospheric electrons for the bi-Maxwellian and kappa source plasma distribution functions. The current-voltage formulas have in principle been well known for a long time, but the kappa energy flux formulas have not appeared in the literature before. We give a unified treatment of the bi-Maxwellian and kappa distributions, correcting some errors in previous work. We give both exact results and two kinds of approximate formulas for the current density and the energy flux. The first approximation is almost generally valid and is practical to compute. The first approximation formulas are therefore suitable for use in simulations. In the second approximation we assume in addition that the thermal energy is small compared to the potential drop. This yields even simpler linear formulas which are suitable for many types of event studies and which have a more transparent physical interpretation than the first approximation formulas. We also show how it is possible to derive the first approximation formulas even for those distributions for which the exact results can not be computed analytically. The kappa field-aligned conductance value turns out always to be smaller than the corresponding Maxwellian conductance. We also verify that the obtained kappa current density and energy flux formulas go to Maxwellian results when k .     

Upward acceleration of magnetospheric ions by oscillatory centrifugal force

The paper addresses the issue of upward acceleration of ions along geomagnetic field lines. It has been shown that ion acceleration by electric field oscillations (formerly known as magnetic moment “pumping” or MMP) may be treated as a centrifugal acceleration mechanism. More precisely, the case in point is oscillatory centrifugal acceleration; this brings up the question on comparing the MMP with the centrifugal acceleration caused by the quasi-static magnetospheric convection field. It has been found that at high geomagnetic latitudes, the oscillatory centrifugal force is weaker or stronger than the centrifugal force of magnetospheric convection if the ratio of the electric field oscillation amplitude to the mean field is correspondingly lower or higher than \(\sqrt 2 \). Analysis of data from measurements and calculations of magnetospheric electric fields suggests that, contrary to current opinion, the oscillatory centrifugal force may be comparable to the centrifugal force of magnetospheric convection and even exceed it when strong global Pc5 pulsations are excited in the magnetosphere.     

Effect of self-weight and vertical acceleration on the behaviour of tall structures during earthquake

The effect of self-weight and vertical ground acceleration during earthquakes on vertical cantilevers has been studied. The input is taken to be a bivariate normal random process, digitally simulated on a computer. The tip deflection, base moment and shear force have been obtained numerically for three structures of different natural frequencies. It is found that the presence of self-weight and vertical ground excitation could alter these three quantities considerably. This leads to the conclusion that with tall structures a refined analysis, similar to the one presented here, is advisable.     

Plutonium oxidation state distributions in the Pacific Ocean during 1980–1981

The concentration of plutonium and its oxidation state distribution have been measured as a function of depth at three locations in the North Pacific Ocean. Concentration profiles were similar to those observed in the same area during 1974 with primary maxima at depths of a few hundred meters below the surface and secondary maxima near the bottom. Oxidation state distribution profiles were similar at the three locations with plutonium about equally divided between the reduced and oxidized forms except near the bottom. There the oxidized form was more abundant and comprised ～ 90% of the total plutonium. No major change in oxidation state occurred at the depths of the shallow concentration maxima suggesting that their formation and persistence were not dependent upon a redox change. The concentration maxima near the bottom coincided with the enhanced abundance of the poorly sorbed oxidized form suggesting that they resulted from the loss of oxidized plutonium from the sediments.     

Estimating rainfall erosivity by aggregated drop size distributions

Rainfall erosivity is defined as the potential of the rain to cause erosion, and it can be represented by rainfall kinetic power. At first in this paper, the raindrop size distributions (DSD) measured by an optical disdrometer located at Palermo in the period June 2006–March 2014 and aggregated for intensity classes, are presented. Then an analysis of raindrop size characteristics is carried out, and the reliability of Ulbrich's distribution, using both the maximum likelihood and momentum estimate parameter methods, is tested. The raindrop size measurements are used to determine the experimental rainfall kinetic power values, which are compared with the ones calculated by a theoretically deduced relationship. This analysis demonstrates that the kinetic power is strictly related to the median volume diameter of DSD. Finally, the reliability of the simplest Marshall and Palmer exponential DSD for estimating the rainfall kinetic power is demonstrated. Copyright © 2015 John Wiley & Sons, Ltd.     

Measurements of meteor smoke particles during the ECOMA-2006 campaign: 1. Particle detection by active photoionization

We present a new design of an in situ detector for the study of meteor smoke particles (MSPs) in the middle atmosphere. This detector combines a classical Faraday cup with a xenon-flashlamp for the active photoionization/photodetachment of MSPs and the subsequent detection of corresponding photoelectrons. This instrument was successfully launched in September 2006 from the Andøya Rocket Range in Northern Norway. A comparison of photocurrents measured during this rocket flight and measurements performed in the laboratory proves that observed signatures are truly due to photoelectrons. In addition, the observed altitude cut-off at 60 km (i.e., no signals were observed below this altitude) is fully understood in terms of the mean free path of the photoelectrons in the ambient atmosphere. This interpretation is also proven by a corresponding laboratory experiment. Consideration of all conceivable species which can be ionized by the photons of the xenon-flashlamp demonstrates that only MSPs can quantitatively explain the measured currents below an altitude of 90 km. Above this altitude, measured photocurrents are most likely due to photoionization of nitric oxide. In conclusion, our results demonstrate that the active photoionization and subsequent detection of photoelectrons provides a promising new tool for the study of MSPs in the middle atmosphere. Importantly, this new technique does not rely on the a priori charge of the particles, neither is the accessible particle size range severely limited by aerodynamical effects. Based on the analysis described in this study, the geophysical interpretation of our measurements is presented in the companion paper by Strelnikova, I., et al. [2008. Measurements of meteor smoke particles during the ECOMA-2006 campaign: 2. results. Journal of Atmospheric and Solar-Terrestrial Physics, this issue, doi:10.1016/j.jastp.2008.07.011].     

1961~2016年全球变暖背景下冰川物质亏损加速度研究

过去几十年间,全球冰川物质亏损的加速趋势日益显著,而这种加速趋势将对全球海平面上升、流域水资源以及冰冻圈灾害等方面产生深远的影响.针对目前关于冰川物质亏损加速度的研究仍然比较贫乏的问题,本研究利用实测冰川物质平衡记录和最新的融合实测资料与大地测量法表面高程变化的冰川物质变化数据,对全球冰川物质亏损加速度进行研究.结果表明,1961~2016年全球冰川物质亏损经历了显著的加速过程.在全球尺度上,冰川物质亏损加速度分别为(5.76±1.35)Gt a^-2(冰量损失加速度)和(0.0074±0.0016)m w.e.a^-2(单位面积冰量损失加速度).在区域尺度上,冰川主要分布区(除南极冰盖边缘地区)的冰量损失加速度大于冰川储量较小的区域,其中阿拉斯加地区的冰量损失加速度最大((1.33±0.47)Gt a^-2).对单位面积冰量变化而言,冰川分布面积较小的区域和几个主要冰川分布区都呈现出较大的冰川消融加速度,其中欧洲中部的冰川单位面积物质亏损的加速度最大((0.024±0.0088)m w.e.a^-2).全球气候变暖是冰川物质亏损加速的主要驱动力.通过对比研究,发现格陵兰冰盖和南极冰盖对全球海平面上升贡献的加速度均大于冰川.本研究将有助于提升对冰川变化机理的认识,为应对冰川变化的影响提供科学依据.     

Effect of the wind acceleration magnitude during the first stages of the wind-wave generation process

Ocean Dynamics - A comprehensive analysis of the wavefield evolution under accelerated wind conditions provides an essential contribution to understanding the wind-wave generation process. A set of...