Mirror instability upstream of the termination shock (TS) and in the heliosheath

We experimentally identify mirror mode (MM) structures in the Voyager 1 heliosheath data for the first time. This is done using the magnetic field data alone. The heliosheath MM structures are found to have the following characteristics: (1) quasiperiodic spacings with a typical scale size of ～57 ρ_p, (2) little or no angular changes across the structures (～3° longitude and ～3° latitude), and (3) a lack of sharp boundaries at the magnetic dip edges. It is demonstrated that the pickup of interstellar neutrals in the upstream region of the termination shock (TS) and quasiperpendicular TS plasma compression are the causes of MM instability during intervals when the IMF is nearly orthogonal to the solar wind flow direction. Concomitant additional injection of pickup ions (PUIs) throughout the heliosheath will lead to further MM amplification. MM structures in planetary magnetosheaths and interplanetary sheaths are discussed for comparative purposes. Multiple sources of free energy are often involved.     

Shielded by the wind: the influence of the interstellar medium on the environment of Earth

We report on the recent studies on the long-term influence of cosmic rays on the Earth's environment. While on short time-scales solar activity is the driver for atmospheric changes suspected to be due to cosmic rays, for long time-scales the heliosphere, i.e. the circumsolar region occupied by the expanding part of the Sun's atmosphere, has to be considered. The heliosphere is identified as an important shield against interstellar influences and hazards. It has been demonstrated by quantitative modelling that a change of the interstellar medium surrounding the heliosphere as a result of the Sun's quasi-Keplerian motion around the galactic center triggers significant changes of planetary environments caused by enhanced fluxes of neutral atoms as well as by the increased cosmic ray fluxes. We give a compilation of recent space science results of interest to the atmospheric science community.     

Laboratory measurements of vortex-induced sediment pickup rates

In the present study,vortices were generated in open channel flow with a cross-flow cylinder installed horizontally near the bed.Sediment pickup rates were then measured over the channel bed downstream the cylinder using a sediment lift.The experimental data show that the pickup rate increases exponentially in the presence of vortices.Two different relationships can be clearly observed between the pickup rate and the maximum root-mean-square (rms) value of the streamwise velocity fluctuation,one for the cylinder-obstructed flow and the other for the unobstructed flow.The results imply that the vortex-induced sediment pickup cannot be explained based on the traditional boundary layer theory.     

Driving Galactic Turbulence by Supernova Explosions

We investigate the general properties of supernova driven interstellar turbulence using local three-dimensional MHD simulations under Galactic conditions. Our model includes the effects of large-scale shear due to Galactic differential rotation, density stratification, compressibility, magnetic fields, heating via supernova explosions and parameterized radiative cooling of the interstellar medium. In addition to investigating isolated supernova explosions we allow for multiple supernovae distributed randomly in the Galactic disc and exponentially in the vertical direction. Single supernova explosions drive a strong shock, the lifetime of which is approximately 2 Myr in our model. This stage is found to be characterized by a kinetic energy spectrum in the diffuse gas with spectral index consistent with k = –2. Large-scale shear and Coriolis force act on the supernova remnant producing some vorticity inside it, but this process was found to be very weak. In the case of multiple supernova explosions, older remnants have an important role causing density fluctuations in the interstellar medium. In this clumpy medium, the propagation velocity of the shock fronts changes due to the changing density, and vorticity is generated. In the absence of these supernova interactions the kinetic energy spectrum shows a relatively wide shock spectrum with spectral index k = –2, but when the supernova interactions become dominant the classical k = –5/3 spectrum is observed.     

Effects of estimating the ionospheric and thermospheric parameters on electron density forecasts

Based on the thermosphere-Ionosphere-Electrodynamics General Circulation Model (TIEGCM), a thermospheric-ionospheric data assimilation and forecast system is developed. Using this system, we estimated the oxygen ions, neutral temperature, wind, and composition by assimilating the simulated data from Formosa Satellite 3/Constellation Observing System for Meteorology, Ionosphere, and Climate (COSMIC) occultation electron density profiles to evaluate their effects on the ionospheric forecast. An ensemble Kalman filter data assimilation scheme and combined state and parameter estimation methods are used to estimate the unobserved parameters in the model. The statistical results show that the neutral and ion compositions are more effective than the neutral temperature and wind for improving the forecast of the ionospheric electron density, whose root mean square errors in the assimilation period decreased by approximately 40%, 30%, and 10% due to the estimations of the neutral composition, oxygen ions, and neutral temperature, respectively. Due to the different physical and chemical processes that these parameters primarily affect, their e-folding times differ greatly from longer than 12 h for neutral composition to approximately 6 h for oxygen ions and 3 h for neutral temperature. The effect of estimating the neutral composition on improving the ionospheric forecast is greater than that of estimating the oxygen ions, which can be also be seen in an actual data assimilation experiment. This indicates that the neutral composition is the most important thermospheric parameter in ionospheric data assimilations and forecasts.     

天然地震识别与震相自动拾取技术进展

震相拾取是地震数据处理过程中最基本的步骤之一。在传统的人工拾取技术不能满足庞大的地震数据处理需求的情况下,震相自动拾取技术从产生到发展至今经历了漫长的过程。本文回顾并总结了震相自动拾取技术的发展状况,重点介绍了长短时窗法、赤池准则法、模板匹配技术、基于自相关盲搜索的FAST法、S波偏振分析法、人工智能方法等,以及近年发展起来的多频率震相识别、全波形叠加、二次方自回归模型等方法,同时分析了每种方法的优势和局限性。     

Origin of the solar wind: Astrophysical and plasma-physical aspects of the problem

At what evolutionary stage of the Sun as a star the accumulation of its matter from the interstellar medium ended and the dominant outflow of solar wind (SW) streams started is one of the main outstanding questions in the astrophysical aspect of the problem of SW origin. It is unknown when and how this happened in detail, although the onset of thermonuclear reactions in the solar interior undoubtedly played a crucial role in the energetics and dynamics of the star, which could lead to such a change of the regimes. Therefore, it is hypothesized that the accretion or plasma outflow from the star was determined by the preceding evolution, i.e., by the “memory“ and not just by the distribution of instantaneous density, temperature, magnetic field, and other macroscopic parameters of the system that consists of this star, its nearest stellar environment, and interstellar gas. Depending on this, neighboring stars can serve as donors or acceptors of interstellar gas. Some of them can simultaneously or alternately play both roles. The polytropic solution for centrally symmetric flows obtained by Bondi is degenerate in the sign of the radial velocity. It is suitable for describing the quasi-stationary regimes of both types. However, the theory of transient processes has not been developed. Hence, the question of whether there exist stars similar in their internal structure and parameters to the present-day Sun but without stellar wind emission or even with interstellar gas accretion can be answered only observationally. The possibility that such stars exist is not ruled out; it does not contradict any laws of nature. The plasma-physical aspect of the problem of SW origin concerns much shorter time intervals than the main evolutionary time scale measured in billions of years. Hence, this aspect of the problem has been studied much better, although it is also fairly complex and has not yet been solved in much detail due to the multi-scale character of the flow formation processes. The SW as a permanent supermagnetosonic plasma outflow in the radial direction appears against the background of much more powerful nonequilibrium and unsteady motions, which are ordered only partially in the upper solar atmosphere and corona (turbosphere). The instantaneous SW state is controlled by the fluxes of free energy, matter, and momentum that enter the corona from the convection zone and underlying solar atmospheric layers. Although the main physical mechanisms of the transport of free energy of the electromagnetic field and plasma are generally well known, they need a quantitative analysis as applied to specific realizations in frequent and rare particle collisions in the solar corona to ascertain the nonlocal processes of the formation of fields and plasma flows, including the SW.     

Effects of atmospheric oscillations on the field-aligned ion motions in the polar F-region

The field-aligned neutral oscillations in the F-region (altitudes between 165 and 275 km) were compared using data obtained simultaneously with two independent instruments: the European Incoherent Scatter (EISCAT) UHF radar and a scanning Fabry-Perot interferometer (FPI). During the night of February 8, 1997, simultaneous observations with these instruments were conducted at Tromsø, Norway. Theoretically, the field-aligned neutral wind velocity can be obtained from the field-aligned ion velocity and by diffusion and ambipolar diffusion velocities. We thus derived field-aligned neutral wind velocities from the plasma velocities in EISCAT radar data. They were compared with those observed with the FPI (=630.0 nm), which are assumed to be weighted height averages of the actual neutral wind. The weighting function is the normalized height dependent emission rate. We used two model weighting functions to derive the neutral wind from EISCAT data. One was that the neutral wind velocity observed with the FPI is velocity integrated over the entire emission layer and multiplied by the theoretical normalized emission rate. The other was that the neutral wind velocity observed with the FPI corresponds to the velocity only around an altitude where the emission rate has a peak. Differences between the two methods were identified, but not completely clarified. However, the neutral wind velocities from both instruments had peak-to-peak correspondences at oscillation periods of about 10–40 min, shorter than that for the momentum transfer from ions to neutrals, but longer than from neutrals to ions. The synchronizing motions in the neutral wind velocities suggest that the momentum transfer from neutrals to ions was thought to be dominant for the observed field-aligned oscillations rather than the transfer from ions to neutrals. It is concluded that during the observation, the plasma oscillations observed with the EISCAT radar at different altitudes in the F-region are thought to be due to the motion of neutrals.     

Lognormal distribution of the observed and modelled neutral thermospheric densities

For analyzing measurements of any kind, it is important to estimate the probability distribution of the measurement errors. When modelling the observations using least-squares fitting, the distribution of the errors plays a vital role in choosing the merit function to be minimized, as unnormally distributed errors (e.g. outliers, or displaying asymmetry around the mean) may substantially skew a least-squares fit of estimated model parameters. Using the CACTUS accelerometer data covering heights of 230–750 km, we will show that the statistical relationship between the commonly used semi-empirical models of neutral thermospheric density (MSIS, DTM) and the observed densities is consistent with lognormal distribution, i.e. the logarithm of the ratio of the measurements to the predictions is approximately normally distributed. This experimental fact may be applied in modelling the neutral thermospheric density. bezdek@asu.cas.cz     

The Uptake of Phosphate Ions by the Alga Hydrodictyon reticulatum

The uptake of orthophosphate has been studied in order to determine the chemical forms of intracellular phosphorus. It was found that the concentration of the main species–orthophosphate and acid hydrolyzable phosphorus–changed in dependence on experimental conditions. The highest uptake of orthophosphate was observed in the neutral medium in the presence of nitrate or ammonium ions in the light, whereas the uptake in the dark was negligible. The uptake of orthophosphate was found to be connected with the transport of alkali metals or ammonium ions into the cell. The rate of the uptake of orthophosphate was compared with that of nitrite, nitrate and ammonium ions.     

Molecules, ices and astronomy

David A Williams, Wendy A Brown, Stephen D Price, Jonathan M C Rawlings and Serena Viti of University College London review how far experimental work on molecular synthesis can be applied to the interstellar medium – and how it is becoming a tool for the understanding of astrophysical processes.     

基于梯度扩散薄膜技术(DGT)的氨基生物炭覆盖沉积物水界面铜、铅释放研究

湖泊沉积物的重金属污染防治一直是环境领域的热点问题.本研究采用氨基生物炭作为覆盖材料,利用梯度扩散薄膜技术(DGT),研究了上覆水不同pH及水流扰动条件下Cu(Ⅱ)、Pb(Ⅱ)在沉积物水界面间的原位释放特征,以及氨基生物炭对湖泊沉积物重金属污染的原位修复效果.研究结果表明,在0 r/min或100 r/min水动力条件下,可移动态重金属离子有不断由沉积物向其他介质扩散的趋势,1.81 kg/m 2的氨基生物炭覆盖强度可降低Cu(Ⅱ)、Pb(Ⅱ)释放通量达89%以上,有效减小了水环境中重金属的潜在生态风险.在pH=5的酸性及pH=9的碱性水环境中原位修复效果较差,水体中大量的H+或络合物均会削弱氨基生物炭对重金属离子的吸附,当上覆水在pH=7的中性条件时原位修复效果最佳.100 r/min水流扰动下的上覆水Cu(Ⅱ)、Pb(Ⅱ)含量在释放平衡时较0 r/min条件下高出0.036~0.096μg/mL,说明高强度的水流扰动易造成覆盖材料的扬起和浮动,导致覆盖材料与重金属发生解吸.     

Imaging a geomagnetic storm with energetic neutral atoms

The ring current during a geomagnetic storm on May 2, 1986 has been modeled using a bounce averaged kinetic equations for the phase space density of hydrogen ions, considering charge exchange and Coulomb losses along the drift path. The resulting equatorial pitch angle distribution is used to generate data simulating the medium and high energy neutral atom imagers to be flown on IMAGE. A method for deconvolving these images is described and applied to the simulated data. The results show that, when there are sufficient counts, the deconvolved distribution contains the main features of the original source and that the energy spectrum at a specific time as well as the total energy of the ring current as a function of time can be extracted from the energetic neutral atom images.     

基于互信息量的地震信号检测和初至提取方法

本文将现代信息科学中的重要基础理论——信息论引入到地震信号的分析和处理中,提出了一种利用互信息量检测地震信号并进行初至提取的方法,给出了该方法的基本原理和具体算法.计算结果表明,互信息量随滑动窗口移动的变化情况可以明确标示出待测地震信号的存在,通过提取互信息量的突变点或峰值点,能够有效拾取地震波的初至时刻.这种方法还可以特别针对非传统的地震信号,如连续随机信号、随机脉冲序列等进行处理.在这些信号条件下,往往信噪比很低,波形随传播距离发生较大变化,传统的信号检测方法效果不佳,而这种以随机信号检测为基础的互信息量探测方法具有很好的性能,很有发展前景.     

释放化学物质耗空电离层电子密度的研究

电离层作为电波传播的主要通道和载体,影响着无线电通信的质量,因此人工电离层扰动具有广阔的应用前景,在电离层中释放具有较强电子亲和力的化学物质可以耗空电离层F区的电子密度,是人工电离层扰动的有效手段之一.本文通过对CO2和SF6气体在电离层中的扩散和离子化学反应过程的分析,理论计算了在我国北京地区上空释放这两种气体后电离...     

Evaluating the hydrological and hydrochemical responses of a High Arctic catchment during an exceptionally warm summer

The Arctic has experienced substantial warming during the past century with models projecting continued warming accompanied by increases in summer precipitation for most regions. A key impact of increasing air surface temperatures is the deepening of the active layer, which is expected to alter hydrological processes and pathways. The aim of this study was to determine how one of the warmest and wettest summers in the past decade at a High Arctic watershed impacted water infiltration and storage in deeply thawed soil and solute concentrations in stream runoff during the thaw period. In June and July 2012 at the Cape Bounty Watershed Observatory, we combined active layer measurements with major ion concentrations and stable isotopes in surface waters to characterize the movement of different runoff sources: snowmelt, rainfall, and soil water. Results indicate that deep ground thaw enhanced the storage of infiltrated water following rainfall. Soil water from infiltrated rainfall flowed through the thawed transient layer and upper permafrost, which likely solubilized ions previously stored at depth. Subsequent rainfall events acted as a hydrological flushing mechanism, mobilizing solutes from the subsurface to the surface. This solute flushing substantially increased ion concentrations in stream runoff throughout mid to late July. Results further suggest the importance of rainfall and soil water as sources of runoff in a High Arctic catchment during mid to late summer as infiltrated snowmelt is drained from soil following baseflow. Although there was some evaporation of surface water, our study indicates that flushing from solute stores in the transient layer was the primary driver of increased ion concentrations in stream runoff and not evaporative concentration of surface water. With warmer and wetter summers projected for the Arctic, ion concentrations in runoff (especially in the late thaw season), will likely increase due to the deep storage and subsurface flow of infiltrated water and subsequent flushing of previously frozen solutes to the surface.     

Localized structure in the cusp and high-latitude ionosphere: a modelling study

The ionospheric signature of a flux transfer event (FTE) seen in EISCAT radar data has been used as the basis for a modelling study using a new numerical model of the high-latitude ionosphere developed at the University of Sheffield, UK. The evolution of structure in the high-latitude ionosphere is investigated and examined with respect to the current views of polar patch formation and development. A localized velocity enhancement, of the type associated with FTEs, is added to the plasma as it passes through the cusp. This is found to produce a region of greatly enhanced ion temperature. The new model can provide greater detail during this event as it includes anisotropic temperature calculations for the O⁺ ions. This illustrates the uneven partitioning of the energy during an event of this type. O⁺ ion temperatures are found to become increasingly anisotropic, with the perpendicular temperature being substantially larger than the parallel component during the velocity enhancement. The enhanced temperatures lead to an increase in the recombination rate, which results in an alteration of the ion concentrations. A region of decreased O⁺ and increased molecular ion concentration develops in the cusp. The electron temperature is less enhanced than the ions. As the new model has an upper boundary of 10 000 km the topside can also be studied in great detail. Large upward fluxes are seen to transport plasma to higher altitudes, contributing to the alteration of the ion densities. Plasma is stored in the topside ionosphere and released several hours after the FTE has finished as the flux tube convects across the polar cap. This mechanism illustrates how concentration patches can be created on the dayside and be maintained into the nightside polar cap.     

Physical mechanism of strong negative storm effects in the daytime ionospheric F2 region observed with EISCAT

A self-consistent method for daytime F-region modelling was applied to EISCAT observations during two periods comprising the very disturbed days 3 April 1992 and 10 April 1990. The observed strong N_e decrease at F2-layer heights originated from different physical mechanisms in the two cases. The negative F2-layer storm effect with an N_mF2 decrease by a factor of 6.4 on 3 April 1992 was produced by enhanced electric fields (E 85 mV/m) and strong downward plasma drifts, but without any noticeable changes in thermos-pheric parameters. The increase of the O⁺ + N₂ reaction rate resulted in a strong enrichment of the ionosphere with molecular ions even at F2-layer heights. The enhanced electric field produced a wide mid-latitude daytime trough on 03 April 1992 not usually observed during similar polarization jet events. The other strong negative storm effect on 10 April 1990 with a complete disappearance of the F2-layer maximum at the usual heights was attributed mainly to changes in neutral composition and temperature. A small value for the shape parameter S in the neutral temperature profile and a low neutral temperature at 120 km indicate strong cooling of the lower thermosphere. We propose that this cooling is due to increased nitric oxide concentration usually observed at these heights during geomagnetic storms.     

Comparative outline of the region of interaction of the solar wind with the Ionosphere of Venus and Mars

The general features of the region of interaction of the solar wind with the ionosphere of Venus and Mars are compared using data obtained with the Mariner 5 and the Pioneer Venus Orbiter (PVO) spacecraft for Venus and with the Phobos II, the Mars Global Surveyor (MGS) and the Mars Express spacecraft for Mars. Despite the overall weak intrinsic global magnetic field that is present in both planets there are significant differences in the manner in which the interplanetary magnetic field accumulates and is organized around and within their ionosphere. Such differences are unrelated to the crustal magnetic field remnants inferred from the MGS measurements around Mars. In fact, while in Venus and Mars there is a region in which the magnetic field becomes enhanced as it piles up in their plasma environment it is shown that such a region exhibits different regimes with respect to changes in the ion composition measured outside and within the ionosphere. At Venus the region of enhanced magnetic field intensity occurs in general above the ionopause which represents the boundary across which there is a change in the ion composition with dominant solar wind protons above and planetary O⁺ ions below. At Mars the region of enhanced magnetic field is located below a magnetic pileup boundary across which there is also a comparable change in the ion composition (solar wind protons above and planetary O⁺ ions below). It is argued that this difference in the relative position of the region of enhanced magnetic field with respect to that of a plasma boundary that separates different ion populations results from the peculiar response of the ionosphere of each planet to the oncoming solar wind dynamic pressure. While at Venus the peak ionospheric thermal pressure is in general sufficient to withhold the incident solar wind kinetic pressure there is a different response in Mars where the peak ionospheric thermal pressure is in general not large enough to deviate the solar wind. In this latter case the ionosphere is unable to force the solar wind to move around the ionosphere and as a result the oncoming electron population can reach low altitudes where it is influenced by neutral atmospheric particles (the solar wind proton population is replaced at the magnetic pileup boundary which marks the upper extent of the region where the interplanetary magnetic field becomes enhanced). Peculiar conditions are expected near the magnetic polar regions and over the terminator plane where the solar wind is directed along the sides of the planet.