Ion acoustic instability of HPT particles,FAC density,anomalous resistivity and parallel electric field in the auroral region

During the magnetic storm of 21st March 1990, the DE-1 spacecraft encountered the auroral region at high invariant latitude at altitudes ranging from a few thousand kilometers in the ionosphere to many earth radii in the magnetosphere. The magnetic field perturbations interpretable as field aligned current (FAC) layers and the electrostatic turbulence possibly due to electrostatic ion acoustic instability driven by these currents are shown. The critical drift velocity of Hot Plasma Torus (HPT) electrons and the growth rate of ion acoustic wave as a function of electron to ion temperature ratio (T _e/T_i) for low and high current densities and energy of HPT electrons are found out. The intense FAC destabilizes the ion acoustic wave and the resultant electrostatic turbulence creates an anomalous resistivity. The current driven resistivity produces parallel electric field and high power dissipation. The anomalous resistivityη, potential difference along the auroral field lines V_t|, intensity of electric field turbulenceE _t| and power produced per unit volumeP are computed. It is found that the change in westward magnetic perturbation increasesJ _t|, η, V_t|, E_t| andP. Hence HPT electrons are heated and accelerated due to power dissipation during magnetically active periods in the auroral region. Concerning, applications, such HPT electrons can be used in particle accelerators like electron ring accelerator, smokatron etc.     

The generation of hard X-rays and relativistic protons observed during solar flares

The flare source of thermal X-rays above a magnetic arch in the corona arises from the dissipation of the magnetic energy of the current sheet formed at the reconnection of magnetic-field lines. The sources of hard X-rays emitted from the footpoints of the magnetic arch are beams of electrons accelerated in field-aligned currents induced by the Hall electric field generated in the current sheet. Both the hard X-rays detected above the active region and the type III radio emission are radiated by electrons accelerated in the field-aligned currents induced by Alfven waves. The solar cosmic rays are emitted promptly at the instant of the flare. It is important that the Lorentz electric field accelerates protons along the singular magnetic X line. The relativistic protons propagate along the interplanetary magnetic field. These protons have exponential spectra, typical for acceleration occurring in current sheets. A mechanism that is relevant for the generation of delayed cosmic rays, which demonstrate significant anisotropy and a power-law spectrum with γ ∼5, is also discussed.     

The generation of magnetic field via convective motions in the photosphere,Alvén waves,and the origin of chromospheric spicules

The basis is laid out for a theory relating various phenomena in the solar atmosphere, including localized concentrations of magnetic field at the bases of coronal magnetic arches, chromospheric spicules, twisted coronal magnetic flux tubes, and flows of energy carried by Alfvén waves propagating upward into the corona. The structure of photospheric currents localized in the vicinity of supergranule boundaries and excited by convective motions is studied. These currents exist primarily in a “dynamo layer” of sharply enhanced transverse conductivity, which forms in the weakly ionized thermal photospheric plasma located in the solar gravitational field. The motions of the electrons and ions in this layer have appreciably different characters: the ions are collisionly driven by the flows of neutral atoms, while the electrons drift in the crossed electric and magnetic fields. The electric field supporting the current arises due to the polarization of the electrons and ions. This field also gives rise to Alfvén perturbations that propagate upward into the corona, together with their associated longitudinal currents. The character of this “loading” makes the system of fields and currents uniquely defined. Moreover, the momentum flux carried by these Alfvén waves should be transferred to the cool chromospheric gas, facilitating the vertical ejection of this gas in the form of spicules, as was first proposed in 1992 by Haerendel.     

电气石的电场效应及其在环境领域中的应用前景

电气石具有永久性的自发电极,电气石微粒的周围存在着以c轴轴面为两极的静电场.在电场作用下,水分子发生电解,形成活性分子 H3O+,吸引水中的杂质、污垢,净化水质;OH- 和水分子结合形成负离子,改善人们的生活环境;电场对带电粒子有吸附作用,可以吸附粉尘,净化空气.电气石还具有高的机械化学稳定性,与沸石、蒙脱石等的吸附作用相比,电气石不具有饱和极限,可持续使用,重复利用率高,在环境领域具有很好的发展前景.     

化能自养型微生物利用太阳能途径的实验研究

针对自然界中天然半导体矿物和化能自养微生物之间的能量交换途径进行了详细的实验研究.半导体光电化学实验结果显示,天然半导体矿物在光照情况下产生的光生电子可将Fe3+还原为Fe2+,其中金红石光催化还原Fe3+的效率为12.5%,闪锌矿为7.86%,该过程通过天然半导体矿物的日光催化作用实现了太阳光能→电能→化学能的转化;控制电势的微生物电化学反应实验结果显示,化能自养型微生物A.f.菌的细胞增加量与外界电子传入而生成的Fe2+的量呈线性关系,且有外来电子传入实验组的A.f.生长量是无电子传入组的441%,该过程通过菌的生长代谢作用实现了化学能→生物质能的转化.进一步的光电化学和微生物电化学耦合实验结果证明,在太阳光和天然半导体矿物共同作用下,A.f.菌的对数生长期由无光时的36 h延长到72 h,同时细菌的生长在该能量转化过程中得到了明显促进.在天然闪锌矿催化条件下,有光条件的A.f.菌数量增加到无光条件的1.90倍;而在金红石催化条件下,有光条件的A.f.菌数量增加到无光条件的1.69倍.实验结果说明,在以天然半导体矿物为媒介的情况下,化能自养微生物可间接利用太阳能来获得自身的生长繁殖所需的能量,这一过程也实现了太阳光能→电能→化学能→生物质能的能量转化途径.     

电气石矿物吸附铜离子试验研究

本文研究了电气石的单晶、电气石微粉对Cu2＋的吸附作用,试验表明：电气石单晶体表面存在着以C轴为两极的静电场,该静电场对Cu2＋的吸附作用效果明显。制备的电气石微粒越细,吸附效果越好。电气石的电场效应使得它在治理污水中Cu2＋污染具有广阔的前景。     

The electric fields of radio pulsars with asymmetric nondipolar magnetic fields

The effect of the curvature of open magnetic field lines on the generation of electric fields in radio pulsars is considered in the framework of a Goldreich-Julian model, for both a regime with a free outflow of electrons from the neutron-star surface and the case of a small thermoemission current. An expression for the electron thermoemission current in a strong magnetic field is derived. The electric field associated with the curvature of the magnetic flux tubes is comparable to the field generated by the relativistic dragging of the inertial frames.     

The appearance of a radio-pulsar magnetosphere from a vacuum with a strong magnetic field. Motion of charged particles

The motion of electrons and positrons in the vacuum magnetosphere of a neutron star with a surface magnetic field of B ≈ 10¹² G is considered. Particles created in the magnetosphere or falling into it from outside are virtually instantaneously accelerated to Lorentz factors γ ≈ 10⁸. After crossing the force-free surface, where the projection of the electric field onto the magnetic field vanishes, a particle begins to undergo ultra-relativistic oscillations. The particle experiences a regular drift along the force-free surface simultaneous with this oscillatory motion.     

Electron acceleration in the ionosphere of Io

A mechanism for the acceleration of electrons in the ionosphere of Io due to the moon's motion through the Jovian magnetic field and the presence of Io's ionosphere is considered. Attention is drawn to the important role of the anisotropic conductivity of the ionosphere, which results in the formation of a longitudinal (with respect to the planetary magnetic field) component of the charge-separation electric field. Owing to this anisotropy, the electric field induced by the motion of Io, E_i, produces in Io's ionosphere not only a Pedersen electrical current along E_i but also a Hall current that is approximately perpendicular to the moon's surface in the “upstream” and “downstream” parts of the ionosphere. However, this current cannot be closed through the surface, leading to the formation of a powerful charge-separation field in Io's ionosphere. This field has a component parallel to the magnetic field, with an amplitude comparable to that of the induced electric field. Electron runaway along the magnetic field is also considered, and the occurrence of “active longitudes” and preferred locations for the sources of decametric radio emission in the northern hemisphere of Jupiter are interpreted. The characteristic energies and fluxes of the accelerated electrons injected into Io's flux tube are estimated. The energy of these electron fluxes is sufficient to produce the electromagnetic radiation observed from Io's magnetic tube.     

The appearance of a radio-pulsar magnetosphere from a vacuum with a strong magnetic field. Accumulation of particles

The motion of electrons and positrons in the vacuum magnetosphere of a neutron star with a surface magnetic field of B ≈ 10¹² G is considered. Particles created in the magnetosphere or falling into it from outside are virtually instantaneously accelerated to Lorentz factors γ ≈ 10⁸. After crossing the force-free surface, where the projection of the electric field onto the magnetic field vanishes, a particle begins to undergo ultra-relativistic oscillations. The particle experiences a regular drift along the force-free surface simultaneous with this oscillatory motion.     

The cyclotron spectrum of anisotropic ultrarelativistic electrons: Interpretation of X-ray pulsar spectra

The spectrum of cyclotron radiation produced by electrons with a strongly anisotropic velocity distribution is calculated taking into account higher harmonics. The motion of the electrons is assumed to be ultrarelativistic along the magnetic field and nonrelativistic across the field. One characteristic feature of the resulting spectrum is that harmonics of various orders are not equally spaced. The physical properties and observed spectra of four X-ray pulsars displaying higher cyclotron harmonics are analyzed. It was shown that at least in one of them, the cyclotron feature can apparently be only an emission line. Moreover, the observed harmonics are not equidistant, and display certain other properties characteristic of emission by strongly anisotropic ultrarelativistic electrons. In addition, there are indirect theoretical arguments that the electrons giving rise to cyclotron features in the spectra of X-ray pulsars are ultrarelativistic and characterized by strongly anisotropic distributions. As a result, estimates of the magnetic fields of X-ray pulsars (which are usually derived from the energies of cyclotron lines) and certain other physical parameters require substantial revision.     

高应力条件下的岩芯电磁性能变化

根据标准晶格模型理论,在高应力作用下,岩石的Si-O键最外层电子将被挤入晶格间隙里,松散外逸的电子云在电场中将产生直流电流（DC）,进而吸收电磁波,转换成交流电流（AC）。直流电流来源于量子力学穿隧效应电子和断键电子。穿隧效应电子的形成过程和原理:氧原子的最外电子被束缚在浅位能井（shallow potential well）（0.38 V）,当高应力作用时,电子吸收部分能量,增加其动能,虽然这种轻微的动能增加不足以使电子克服并跳出它的位能井（potential well）,但它足以增加穿过井壁（well wall）进入晶格空隙间的概率,这个概率乘以可用氧原子的数目即为由于隧穿效应形成电子云的电子数量,其量级通常为微微库伦（picocoulombs）到纳米库伦（nanocoulombs）。断键电子的形成过程和原理:从微裂纹开始断裂键释放电子,并且裂纹成核点极可能开始是平行排列的,每当Si-O键断裂时,就会产生一个+Si悬键,伴随着一个自由电子附着在-O原子上,这个电子将从原子跃迁到原子,这种电子电流与裂纹的表面积和电池电极的收集效率成正比。断键形成的电子云比穿隧效应多很多。两种电子均被试验所证实。在高应力条件下岩石破裂之前,由电子穿隧效应,DC缓慢增加,随着岩石破裂的发生而导致断键电子增多,DC急剧增加;AC的电压振幅（V）随电流（I）增大而减小,当电流减小到正常时,在岩石破裂后电压振幅回归正常;遵守能量守恒原理,吸收的电磁波能量（E）与交流电流功率（V×I）相等,即E=V×I。研究结果表明电磁波监测可用于探测地壳高应力变化和岩石破裂特征,当应力达到岩体断裂的临界强度时,其应变晶体结构开始释放越来越多的外逸电子,最终岩体晶体结构断裂产生一个地震或滑动事件。岩石破裂的电磁性能变化研究可用于研发电磁波地学监测仪器,电磁波监测可以作为地应力监测的一种补充和对比分析方法,两种方法相结合比地应力监测一种方法更可靠。此外,在高应力条件下岩石还有其它现象:应变蠕变辐射、光发射、声发射、静电等,这些现象的观测也是预测地质事件需要考虑的条件。      

Drift loss cone instability in the ring current and plasma sheet

The drift loss cone instability, propagating nearly transverse to the ambient magnetic field, is studied in the ring current plasma taking into account the relative driftU between electrons and protons due to density gradients. The growth rates attain maxima and then decrease as the wave number parallel to the magnetic fieldk _II increases. The peak values of the growth rates, maximised with respect tok _II, are enhanced by the increase in number density, electron temperature and loss cone index, and by the decrease in β_t, the ratio of the proton thermal pressure to magnetic field pressure. The unstable frequencies fall in the range of 5 to 30Ω_p with the growth rate γ ≥Ω_p. In the ring current region betweenL=4 and 5, the instability will generate a strong turbulence in the frequency range between 5–500 Hz which can produce fluctuating electric fields 0. 5–5 mV/m and magnetic field 0.8–80mγ. This instability can also occur on the auroral field lines, which connect to the region of intense earthward plasma flow in the distant magnetotail and produce a broad band electrostatic noise.     

Distribution of the potential and concentration of electrons in low-temperature plasma with hollow microparticles

Using approximation of a uniform background (the jellium model) for a condensed dispersed phase, the analytical expressions describing a spatial distribution of the potential of the electric field and electron concentration in the low-temperature plasma at equilibrium which contains hollow spherical microparticles are obtained. The influence of heating temperature of plasma on the above distributions is studied, and the dependencies of the charge on microparticle radius, the size of the microparticle cavity and the absolute temperature of plasma are calculated. It is shown that electrons can be emitted not only into the surrounding plasma but also into the cavity of the particles.     

我国萤石资源现状及展望

萤石由于其独特的物理、化学性质，主要用于钢铁、化工、建材三大行业。近年来，化工行业已成为萤石的最大用户。尤其在氟化工方面，用以制造氢氟酸及其衍生物，特别是氟碳化合物，更广泛地应用于各工业部门。不同行业对萤石的质量要求不同，有各自的标准。作为我国外贸的创汇产品，对萤石资源的进一步开发工作仍需重视，制酸级萤石在氟化工生产方面尚具发展潜力。     

Comparing the adaptive Gaussian mixture filter with the ensemble Kalman filter on synthetic reservoir models

Over the last years, the ensemble Kalman filter (EnKF) has become a very popular tool for history matching petroleum reservoirs. EnKF is an alternative to more traditional history matching techniques as it is computationally fast and easy to implement. Instead of seeking one best model estimate, EnKF is a Monte Carlo method that represents the solution with an ensemble of state vectors. Lately, several ensemble-based methods have been proposed to improve upon the solution produced by EnKF. In this paper, we compare EnKF with one of the most recently proposed methods, the adaptive Gaussian mixture filter (AGM), on a 2D synthetic reservoir and the Punq-S3 test case. AGM was introduced to loosen up the requirement of a Gaussian prior distribution as implicitly formulated in EnKF. By combining ideas from particle filters with EnKF, AGM extends the low-rank kernel particle Kalman filter. The simulation study shows that while both methods match the historical data well, AGM is better at preserving the geostatistics of the prior distribution. Further, AGM also produces estimated fields that have a higher empirical correlation with the reference field than the corresponding fields obtained with EnKF.     

地电化学提取法在金银矿上的应用效果

地电化学提取法(简称电提取)是一种物理化学相结合,以离子晕为基础的找矿方法,即用人工电场力富集,提取自然状态的微量离子晕中的元素信息,以达到直接找矿或区分物化探异常源性质为目的新兴找矿特效方法.我单位在90年代初引进此方法以来分别在辽宁省阜新排山楼金矿、盖县猫岭金矿、开原市李家银矿、北票二道沟金矿等已知矿床上进行了方法试验研究,并取得较好的找矿效果.在阜新排山楼金矿已知矿体上的方法试验结果对比,在已知金矿外围双山地段,通过做电提取金矿勘查工作,发现电提取金异常带,经槽探工程揭露发现平均品位1.05×10^-6,最高品位2.4×10^-6的含金矿化体,经打钻验证,在深部发现工业矿体,现今成为中型金矿.通过对收集的国内外和我单位电提取实地勘查资料的分析研究,总结出在典型金、银矿电提取找矿规律.     

Significance of conditioning to piezometric head data for predictions of mass transport in groundwater modeling

Transmissivity and head data are sampled from an exhaustive synthetic reference field and used to predict the arrival positions and arrival times of a number of particles transported across the field, together with an uncertainty estimate. Different combinations of number of transmissivity data and number of head data used are considered in each one of a series of 64 Monte-Carlo analyses. In each analysis, 250 realizations of transmissivity fields conditioned to both transmissivity and head data are generated using a novel geostatistically based inverse method. Pooling the solutions of the flow and transport equations in all 250 realizations allows building conditional frequency distributions for particle arrival positions and arrival times. By comparing these fresquency distributions, we can assess the incremental gain that additional head data provide. The main conclusion is that the first few head data dramatically improve the quality of transport predictions.     

Magnetic fields of telluric currents and mapping upper portions of crust

The author proposes a method of telluric-magnetic mapping, profiling, and exploration. The profiling involves recording of short-period variations in the telluric current and the magnetic field (MTP) and an areal (MVR), similar to the above. The method can be used on any segment of the crust, especially with newly designed, highly sensitive short-period magnetometer. The magnetic fields of telluric currents are measured by means of a four-channel oscillograph controlled from a panel in which switches are incorporated. The magnetic fields of the telluric current are measured at two points, since the automatic switching arrangement permits a procedure identical with the measurements in the telluric current. Amplitudes and periods of almost sinusoidal waves are measures of the chords of the elliposidal electric and magnetic fields. Analysis of magnetic field mapping and its results are given. The author feels that the telluric-magnetic profiling should replace direct telluric voltage measurements in many regions because of its economics. It gives precise data on the structure of the sedimentary cover. Telluric-exploration will open up entirely new possibilities in permafrost zones and the method will be substantially more efficient than direct telluric measurements. — A.W. Bellais     

The radio sources CTA 21 and OF+247: The hot spots of radio galaxies

The physical conditions in the radio sources CTA 21 and OF+247 are studied assuming that the low-frequency spectral turnovers are due to synchrotron self-absorption. The physical parameters of the radio sources are estimated using a technique based on a nonuniform synchrotron source model. It is shown that the magnetic-field distributions in the dominant compact components of these radio sources are strongly inhomogeneous. The magnetic fields at the center of the sources are B ～ 10^?1 G, and the fields are two to three orders of magnitude weaker at the periphery. The magnetic field averaged over the compact component is B ～ 10^?3 G, and the density of relativistic electrons is n _e ～ 10^?3 cm^?3. Assuming that there is equipartition of the energies of the magnetic field and relativistic particles, averaged over the source, 〈E _H 〉 = 〈E _e 〉 ～ 10^?7–10^?6 erg cm^?3. The energy density of the magnetic field exceeds that of the relativistic electrons at the centers of the radio sources. The derived parameters of CTA 21 and OF+247 are close to those of the hot spots in the radio galaxy Cygnus A. On this basis, it is suggested that CTA 21 and OF+247 are radio galaxies at an early stage of their evolution, when the hot spots (dominant compact radio components) have appeared, and the radio lobes (weak extended components) are still being formed.