三维强朗缪尔湍动对电子的加速

从等离子体动力学理论出发，研究了三维强朗缪尔湍动对电子的加速，得出了高能电子的能量谱，理论得出的这种能量谱能够跟实验观测结果很好的吻合。     

低速太阳风中电子的随机湍动加热

在低速太阳风中,在离子声波湍动已经激发的区域,可以产生沿着一定方向运动的逃兔电子束,该电子束可以激发起强烈的纵等离子激元的湍动,朗缪尔波的主要吸收机制是通过等离子体热电子的非线性散射,朗缪尔波受激转换为离子声波,这种转换随着电子的迅速加热,几乎所有有纵等离子激元的能量都转移给散射电子,导致低速太阳风中电子的温度高于质了的温度。     

光学厚的介质中同步辐射谱

文章利用等离子体中湍动波谱计算公式得到,在光学厚的介质中麦克斯韦分布的极端相对论电子在磁场中产生的同步加速辐射谱为瑞利-金斯谱。代入太阳活动区物理量的特征值,经过计算分析发现该谱对太阳耀斑过程中少数快电子的加速是有效的,而对基础等离子体的加热的贡献很小。     

高速太阳风中的α粒子流

利用等离子体湍动理论，研究α粒了在高速太阳风中，被阿尔文波湍动随机加速的机制，定量地解释了α粒子的速度大于质子的速度，α粒子的温度高于质了的温度的原因。     

高速太阳风中质子的随机湍动加热

在高速太阳风中，Ａｌｆｖｅｎ波在传播过程中其能量可能转移给快磁声波，当磁场强度和Ａｌｆｖｅｎ波速度趋于零时，快磁声波将转变为离子声波。通过对质子的随机湍动加热，而导致高速太阳风中质子平均温度高于电子的平均温度。     

微波等离子体的朗缪尔探针测量

随着微波等离子体的应用越来越广泛,其参数的测量研究也逐渐得到人们的重视.本文使用朗缪尔探针测量了微波等离子体的单探针I-V特性,并根据探针测量原理计算出等离子体空间电位、电子温度,电子密度和离子密度等参数.     

束离子与离子声波准线性相互作用的研究

给出了束离子与离子声波准线性相互作用的数值解,由解出的波谱进一步给出湍动加速中的加速系数、脉动加速系数、粒子与湍动场间的等效碰撞频率,通过粒子与湍动场间的等效碰撞频率和粒子间有效碰撞频率的比较,说明在有较强湍动场的情形下采用无碰撞等离子体模型是很合适的。     

液-液传质过程中液滴内界面湍动现象

在水-丙酮-甲苯和水-丙酮-甲基异丁酮两种液-液体系中,使用放大投影法,在包括Rayleigh对流影响和排除Rayleigh对流影响的情况下,观察了溶质在液滴与连续相之间传质引发的界面湍动现象,结果表明,液-液传质过程中液滴内部的界面湍动强烈,对传质有强烈的促进作用.Marangoni对流单独作用下的液滴内部界面湍动强度大,可充满整个液滴内部,而当Marangoni对流与Rayleigh对流耦合存在时,液滴内部界面湍动强度较小,仅存在于液滴界面内侧附近,不能充满整个液滴内部空间.     

ECR放电中电子能量分布函数的确定

在ECR放电实验中，我们测量了简单镜中捕获的电子能量分布函数，通过测量双延迟势，可获得ECR放电中电子在磁镜装置镜喉区域的电子能量分布函数，利用光谱变分和朗缪尔探针可以确定电子分布函数的某些参数，放电是在氩气中进行的，实验中发现，不同的等离子体态有不同的分布函数，它们呈现出指数分布与幂分布。     

太阳活动区参量与太阳耀斑和太阳质子事件的相关性统计分析

太阳黑子活动区与太阳耀斑和太阳质子事件的发生有紧密的关系.选取活动区特征参量包括太阳黑子群面积,磁分类,McIntosh分类,10 cm射电流量,统计和耀斑发生的产率关系;还统计了太阳活动区的位置,软X射线通量和质子事件的产率关系.对于磁分类,McIntosh分类的每一种分类类型计算了耀斑产率,对黑子群面积和10 cm射电流量和软X射线通量用函数拟合了它们和太阳耀斑和太阳质子事件的产率关系.对活动区位置采用了分段统计质子事件产率的方法.统计结果显示我们选取的活动区特征参量与太阳耀斑和质子事件有较强的相关性.统计结果可作为以后建立太阳耀斑,太阳质子事件预报模型中预报因子的选取的基础.     

Energetic particle radiations measured by particle detector on board CBERS-1 satellite

Using the data measured by energetic particle detector on board CBERS-01 and -02 for the past five years, statistics was made to show the general features of MeV electrons and protons along a solar synchronous orbit at an altitude of 780 km. This height is in the bottom region of the Earth's radiation belts. Detectors are inside the satellite cabinet and such continuous monitoring of particle radiation environment inside a satellite has seldom conducted so far. After a proper and careful treatment, it is indicated that the data inside satellite are well correlated with the radiation environment outside. Be-sides the agreement of the general distribution characteristics of energetic electrons and protons with similar observations from other satellites, attention is particularly paid to the disturbed conditions. Variations of particle fluxes are closely related with solar proton events, in general, electron fluxes of outer belt are well correlated with Dst index after three days' delay while the electron injection occurred almost at the same day during great magnetic storms. It is confirmed that both energetic electrons and protons appear in the Polar Cap region only after the solar proton events.     

Monoenergetic beams of relativistic electrons from intense laser-plasma interactions

High-power lasers that fit into a university-scale laboratory can now reach focused intensities of more than 10(19) W cm(-2) at high repetition rates. Such lasers are capable of producing beams of energetic electrons, protons and gamma-rays. Relativistic electrons are generated through the breaking of large-amplitude relativistic plasma waves created in the wake of the laser pulse as it propagates through a plasma, or through a direct interaction between the laser field and the electrons in the plasma. However, the electron beams produced from previous laser-plasma experiments have a large energy spread, limiting their use for potential applications. Here we report high-resolution energy measurements of the electron beams produced from intense laser-plasma interactions, showing that--under particular plasma conditions--it is possible to generate beams of relativistic electrons with low divergence and a small energy spread (less than three per cent). The monoenergetic features were observed in the electron energy spectrum for plasma densities just above a threshold required for breaking of the plasma wave. These features were observed consistently in the electron spectrum, although the energy of the beam was observed to vary from shot to shot. If the issue of energy reproducibility can be addressed, it should be possible to generate ultrashort monoenergetic electron bunches of tunable energy, holding great promise for the future development of 'table-top' particle accelerators.     

A gamma-ray burst with a high-energy spectral component inconsistent with the synchrotron shock model

Gamma-ray bursts are among the most powerful events in nature. These events release most of their energy as photons with energies in the range from 30 keV to a few MeV, with a smaller fraction of the energy radiated in radio, optical, and soft X-ray afterglows. The data are in general agreement with a relativistic shock model, where the prompt and afterglow emissions correspond to synchrotron radiation from shock-accelerated electrons. Here we report an observation of a high-energy (multi-MeV) spectral component in the burst of 17 October 1994 that is distinct from the previously observed lower-energy gamma-ray component. The flux of the high-energy component decays more slowly and its fluence is greater than the lower-energy component; it is described by a power law of differential photon number index approximately -1 up to about 200 MeV. This observation is difficult to explain with the standard synchrotron shock model, suggesting the presence of new phenomena such as a different non-thermal electron process, or the interaction of relativistic protons with photons at the source.     

Si在Au(111)面的电子结构和光学性质的第一性原理研究

基于第一性原理,对Si原子在Au(111)表面和体内掺杂的电子结构和光学性质进行了比较研究。结果表明,在Au(111)体内掺杂时,Si原子与周围六个Au原子成键,p电子更局域。电荷密度分析表明,掺杂Si后,Au原子周围的电子密度明显减少,而SiAu原子之间的电子密度明显增加,电子由Au原子向SiAu原子之间转移。通过计算Mul-liken键级表明,SiAu原子之间形成共价键,表面掺杂时的SiAu键级比体内大。吸收谱的计算表明,在体内掺杂Si原子时的吸收谱明显增强。     

Extremely fast acceleration of cosmic rays in a supernova remnant

Galactic cosmic rays (CRs) are widely believed to be accelerated by shock waves associated with the expansion of supernova ejecta into the interstellar medium. A key issue in this long-standing conjecture is a theoretical prediction that the interstellar magnetic field can be substantially amplified at the shock of a young supernova remnant (SNR) through magnetohydrodynamic waves generated by cosmic rays. Here we report a discovery of the brightening and decay of X-ray hot spots in the shell of the SNR RX J1713.7-3946 on a one-year timescale. This rapid variability shows that the X-rays are produced by ultrarelativistic electrons through a synchrotron process and that electron acceleration does indeed take place in a strongly magnetized environment, indicating amplification of the magnetic field by a factor of more than 100. The X-ray variability also implies that we have witnessed the ongoing shock-acceleration of electrons in real time. Independently, broadband X-ray spectrometric measurements of RX J1713.7-3946 indicate that electron acceleration proceeds in the most effective ('Bohm-diffusion') regime. Taken together, these two results provide a strong argument for acceleration of protons and nuclei to energies of 1 PeV (10(15) eV) and beyond in young supernova remnants.     

Capture of hydroxymethylene and its fast disappearance through tunnelling

Singlet carbenes exhibit a divalent carbon atom whose valence shell contains only six electrons, four involved in bonding to two other atoms and the remaining two forming a non-bonding electron pair. These features render singlet carbenes so reactive that they were long considered too short-lived for isolation and direct characterization. This view changed when it was found that attaching the divalent carbon atom to substituents that are bulky and/or able to donate electrons produces carbenes that can be isolated and stored. N-heterocyclic carbenes are such compounds now in wide use, for example as ligands in metathesis catalysis. In contrast, oxygen-donor-substituted carbenes are inherently less stable and have been less studied. The pre-eminent case is hydroxymethylene, H-C-OH; although it is the key intermediate in the high-energy chemistry of its tautomer formaldehyde, has been implicated since 1921 in the photocatalytic formation of carbohydrates, and is the parent of alkoxycarbenes that lie at the heart of transition-metal carbene chemistry, all attempts to observe this species or other alkoxycarbenes have failed. However, theoretical considerations indicate that hydroxymethylene should be isolatable. Here we report the synthesis of hydroxymethylene and its capture by matrix isolation. We unexpectedly find that H-C-OH rearranges to formaldehyde with a half-life of only 2 h at 11 K by pure hydrogen tunnelling through a large energy barrier in excess of 30 kcal mol(-1).     

A current filamentation mechanism for breaking magnetic field lines during reconnection

During magnetic reconnection, the field lines must break and reconnect to release the energy that drives solar and stellar flares and other explosive events in space and in the laboratory. Exactly how this happens has been unclear, because dissipation is needed to break magnetic field lines and classical collisions are typically weak. Ion-electron drag arising from turbulence, dubbed 'anomalous resistivity', and thermal momentum transport are two mechanisms that have been widely invoked. Measurements of enhanced turbulence near reconnection sites in space and in the laboratory support the anomalous resistivity idea but there has been no demonstration from measurements that this turbulence produces the necessary enhanced drag. Here we report computer simulations that show that neither of the two previously favoured mechanisms controls how magnetic field lines reconnect in the plasmas of greatest interest, those in which the magnetic field dominates the energy budget. Rather, we find that when the current layers that form during magnetic reconnection become too intense, they disintegrate and spread into a complex web of filaments that causes the rate of reconnection to increase abruptly. This filamentary web can be explored in the laboratory or in space with satellites that can measure the resulting electromagnetic turbulence.