SIS/LPB/PAn导电橡胶复合物

采用原位聚合法,在SIS(苯乙烯-异戊二烯-苯乙烯嵌段共聚物)/LPB(液体聚丁二烯)橡胶基体中合成PAn(聚苯胺),形成单面导电的导电橡胶复合物.研究了基体聚合物交联度、苯胺、氧化剂用量和聚合反应时间等几种主要反应条件对复合物导电性的影响.导电层中PAn含量只有6.1%,导电面电导率就可达5.5S/m.该复合物的电导率:①随基体聚合物的交联度的增大而减小;②随苯胺用量的增大而增大;③随氧化剂用量的增大先增大后减小.      

磷酸掺杂型高温质子交换膜燃料电池关键材料研究进展

高温质子交换膜燃料电池(HT-PEMFC)由于较高的工作温度(130~220℃),具有较快的电极反应动力学、较强的抗燃料/空气中杂质毒化能力、广泛的燃料来源(甲醇重整气、工业副产氢等)及简单的水/热管理系统等优点。因此,HT-PEMFC将成为聚合物膜燃料电池的重要前沿发展方向之一。重点介绍了北京航空航天大学团队近十年来在HT-PEMFC关键材料-高温膜、催化层和膜电极等方面的研究进展,针对磷酸(PA)掺杂型高温膜的质子传导率和机械性能之间的最佳平衡点、催化层中PA分布和迁移对电池性能的影响机制,以及大尺寸膜电极一致性对电堆性能影响与衰减机制等科学问题,从聚电解质膜材料的分子设计、有序催化层结构调控和大尺寸膜电极电堆优化等工作进行了梳理,对HT-PEMFC技术所面临的技术挑战问题与未来发展趋势做出了评述和展望。      

Comparison of ion composition from the goddard comprehensive ionosphere database with the international reference ionosphere model

We compared the IRI values of T_e, N_e, T_i, O⁺, H⁺, He⁺, O₂₊, and NO⁺ with AE-C values, obtained from the Goddard Comprehensive Ionosphere Database (GCID), composed of data from the satellites, AE-B, OGO-6, ISIS-2, AE-C, AE-D, and AE-E. O⁺ - H⁺ transition levels were derived from the IRI and AE-C altitude profiles. Some discrepancies were found between IRI and the AE-C data. The IRI electron density was found to be about a factor of 2 higher than the data. The H⁺ composition agreed best among the IRI ions, with an average AE-C/IRI ratio of 1.05. The temperatures of both electrons and ions agreed quite well: the average ratios of AE-C/IRI was found to be .99 for electrons and 1.17 for ions.     

Relative abundance of H and He in outer ionosphere

A mathematical model is used to study the relative abundance of H⁺ and He⁺ ions in the topside ionosphere. It is found that the daytime light-ion densities are strongly coupled with the neutral densities. This fact arises difficulties in modelling the ion composition for IRI without taking into account any particular reference atmosphere. As an example, the transition heights between O⁺---H⁺ and O⁺---He⁺ are shown, plotted against the neutral densities. The supposed linear dependance gives a clear evidence that all light-ion ionization below these heights will experience stronger influence by the neutral atmosphere.     

Auroral signatures of transient processes in the outer magnetosphere

We present an analysis of sporadic and recurrent injections of magnetospheric ions in the midnight auroral oval during substorms and of the associated ionospheric ion outflows. The source of plasma sheet precipitating ions is determined using a simple method, based on the measured relation between the ion inverse velocity and time (l = v × t). This method is applied here to two typical passes of the Interball-Auroral (IA) satellite at distances of 3 R_E above the auroral regions. Substorm related ion injections are shown to be mainly due to time of flight effects. In contrast with particle trajectory computations (Sauvaud et al., 1999), the inverse velocity method does not require magnetic and electric field models and can thus be used systematically for the detection of time of flight dispersed ion structures (TDIS). This allowed us to build a large database of TDIS events and to perform a statistical analysis of their spatial distribution. For the cases presented here the source region of the injected ions is found at radial distances from 18 to 30 R_E near the equatorial magnetosphere. At Interball altitudes ( 3 R_E), ion injections detected at the poleward boundary of the nighside auroral oval are associated with shear Alfvén waves superimposed over large-scale quasi-static current structures. We show that the most poleward TDIS are collocated with a large outflow of ionospheric H⁺ and O⁺ displaying pitch-angle distributions peaked in the pitch-angle range 90°–120°. These ions are thus accelerated perpendicularly to the magnetic field not only in the main auroral acceleration region but also up to at least 3 R_E. The expanding auroral bulge thus constitutes a significant source of H⁺ and O⁺ ions for the mid-tail magnetosphere.     

Evaluation of gravity-dependent membrane potential shift in Paramecium.

It is still debated whether or not gravity can stimulate unicellular organisms. This question may be settled by revealing changes in the membrane potential in a manner depending on the gravitational forces imposed on the cell. We estimated the gravity-dependent membrane potential shift to be about 1 mV G⁻¹ for Paramecium showing gravikinesis at 1–5 G, on the basis of measurements of gravity-induced changes in active propulsion and those of propulsive velocity in solutions, in which the membrane potential has been measured electrophysiologically. The shift in membrane potential to this extent may occur from mechanoreceptive changes in K⁺ or Ca²⁺ conductance by about 1% and might be at the limit of electrophysiological measurement using membrane potential-sensitive dyes. Our measurements of propulsive velocity vs membrane potential also suggested that the reported propulsive force of Paramecium measured in a solution of graded densities with the aid of a video centrifuge microscope at 350 G was 11 times as large as that for −29 mV, i.e., the resting membrane potential at [K⁺]_o = 1 mM and [Ca²⁺]_o = 1 mM, and, by extrapolation, that Paramecium was hyperpolarized to −60 mV by gravity stimulation of 100- G equivalent, the value corrected by considering the reduction of density difference between the interior and exterior of the cell in the graded density solution. The estimated shift of the membrane potential from −29 mV to −60 mV by 100- G equivalent stimulation, i.e., 0.3 mV G⁻¹, could reach the magnitude entirely feasible to be measured more directly.     

The ion energy spectra in the ring current during the geomagnetic storm of February, 1986

Using data from the CHEM instrument on the AMPTE/CCE spacecraft, we follow the development of the ring current energy spectra (1–300 keV/e) of the ion species H⁺, O⁺, He⁺, and He⁺⁺ in the post-noon and pre-noon local time sectors during the geomagnetic storm of February 1986. By comparing displays of phase space density, f, vs. magnetic moment, μ, we can distinguish between enhancements due to newly injected ions and those due to adiabatic energization of a pre-existing population. In both the local time sectors, the initial drop in Dst is associated with enhanced phase space densities of all species. The spectra observed during the pass when the Dst dropped to a minimem of −312 nT show a strong local time asymmetry. In the post-noon sector, the spectra showed the influx of a new population of ions, rich in O⁺ and He⁺⁺. In the pre-noon sector, the flux increase was consistent with adiabatic energization of the ion population injected earlier in the storm. This local time difference is consistent with a greatly enhanced convection electric field which brings a new population from the magnetotail to the post-noon, but not the pre-noon local time sector.     

Diurnal variations of ion flux intensity on a synchronous orbit

The data from the synchronous-orbit satellites of the Gorizont series are used to study the dependences of the ion flux variation amplitudes in the synchronous altitude region (the diurnal behaviour) on particle energies and on the form and rigidity of the particle energy spectrum. The proton fluxes were measured in the energy range E 60–120 keV, and the [N,0]²⁺ and [C,N,0]⁴⁺ ion fluxes in the energy range E 60–70 keV/e.

The ratio of the diurnal variation amplitudes of the studied ions is shown to correspond to the similarity of their energy spectra in the E/Q representation. The magnetically-quiet time gradient of the distribution function F(μ,J,L) in the synchronous-orbit region is shown to be (∂F/∂L)=0 for the H⁺ and [N,0]²⁺ ions and (∂F/∂L) > 0 for the [C,N,0]⁴⁺ ions (at the values of μ corresponding to the examined energy ranges). During magnetically-disturbed periods the inner boundary of the (∂F/∂L)=0 region shifts to lower L and (∂ F/∂L) = O in the synchronous altitude region must be also for the [C,N,O]⁴⁺ ions.     

Photochemistry of planetary ionospheres

The basic photochemical processes in the upper atmospheres and ionospheres of the various bodies in our solar system (planets, moons and comets) are similar. However, there are many different factors (e.g. gas composition, energy input, gravity) which control/change the relative importance of these controlling processes. The photo-chemistry of the inner planets is reasonably well understood at this time, thus there is good agreement between model calculations and most of the observational data base. The extremely limited information that we have available on the ionospheres of the outer planets leads to significant uncertainties about some of the controlling processes. Some important questions (e.g. Is the charge exchange process H⁺ + H₂(v≥4) → H₂⁺ + H important? Is water vapor influx from the rings important?) remain unanswered at this time. In cometary atmospheres the freshly evaporated parent molecules are rapidly photodissociated and photoionized, therefore most of the chemical kinetics of cometary ionospheres involve these rapidly moving and highly reactive ions and radicals.     

超临界压力RP-3在竖直细圆管内混合对流研究

研究了超临界压力下碳氢燃料航空煤油RP-3在竖直细圆管内混合对流,分析了浮升力及热物性对碳氢燃料在垂直管中对流换热的影响。实验中控制热流密度从200~500 kW/m2变化,进口压力变化范围为3~5 MPa,进口雷诺数从5 000~10 500范围内变化。研究表明:在向上流动情况中进口段存在较为明显的入口效应,换热出现恶化现象,而在向下流动中未出现;对于向上和向下流动,由于热物性的综合影响,换热系数沿流动方向增大;在较低进口雷诺数(Re=5 700)时,对于向下流动,随着浮升力影响的增大,浮升力改变了流体径向速度分布,出现了换热强化;在较高进口雷诺数(Re=10 500)时,浮升力对换热的影响依然显著;判别式Bo*数小于5.6×10-7未能预测浮升力对碳氢燃料换热影响。      

内增湿式质子交换膜燃料电池堆动态传热模型

建立了质子交换膜燃料电池阴极的传质模型,综合考虑了影响电堆传热的多个因素,在此基础上针对内增湿式燃料电池堆建立了动态传热模型.采用Runge-Kutta-Felhberg法对模型进行求解,对电流、反应物过量系数、压强、冷却水流量等对电堆温度的影响进行了研究.结果表明,当电流大于25A时电堆温度将不能自行稳定在80℃以下,采用水冷可以有效地将电堆温度控制在较理想的范围内.在额定功率为5kW的燃料电池堆试验台架上进行了热管理试验,试验结果同模型预测值吻合较好.     

Hot hydrogen and deuterium in the exosphere of Venus

A theoretical study of the production, thermalization and escape, of hot atomic hydrogen and deuterium in the exosphere of Venus is presented. The approach adopted involves the quantum mechanical calculation of the charge exchange collision cross sections for (H⁺, H) and (D+, H) collisions, the production of translationally energetic atoms, and their ensuing thermalization and escape from Venus. A kinetic theory which employs the quantum mechanical collision cross sections and accounts for the production, thermalization and escape of hot atoms is described. Preliminary numerical results for escape fluxes calculated with density and temperature profiles as provided from the Pioneer Venus orbiter are presented.