强朗缪尔湍动与太阳质子电子事件

在空间探测中,太阳质子事件都伴生非相对论性电子,却常有观测到电子流而无质子成分的纯电子事件.纯电子事件中,电子流量比通常电子事件低一个量级左右.荷电粒子会因为与强朗缪尔湍动的相互作用而得到加速,经过理论推导发现电子和质子能否得到加速与朗缪尔湍动强度有关.代入日冕活动区物理量的典型值,计算发现正是由于质子和电子的加速条件对朗缪尔湍动强度的要求不同而产生了上述现象.     

"资源一号"卫星星内高能粒子探测器

对空间辐射环境的效应以及“星内高能粒子探测器”原理和设计做了简要而全面地介绍，引用太阳活动宁静时期和一次剧烈的太阳扰动事件期间本仪器的观测数据显示了资料的质量和可用性。     

Fast acceleration of “killer” electrons and energetic ions by interplanetary shock stimulated ULF waves in the inner magnetosphere

Energetic electrons and ions in the Van Allen radiation belt are the number one space weather threat. Understanding how these energetic particles are accelerated within the Van Allen radiation belt is one of the major challenges in space physics. This paper reviews the recent progress on the fast acceleration of "killer" electrons and energetic ions by ultralow frequency (ULF) waves stimulated by the interplanetary shock in the inner magnetosphere. Very low frequency (VLF) wave-particle interaction is considered to be one of the primary electron acceleration mechanisms because electron cyclotron resonances can easily occur in the VLF frequency range. Recently, using four Cluster spacecraft observations, we have found that, after interplanetary shocks impact the Earth’s magnetosphere, energetic electrons in the radiation belt are accelerated almost immediately and continue to accelerate for a few hours. The time scale (a few days) for traditional acceleration mechanisms, based on VLF wave-particle interactions to accelerate electrons to relativistic energies, is too long to explain our observations. Furthermore, we have found that interplanetary shocks or solar wind pressure pulses, with even small dynamic pressure changes, can play a non-negligible role in radiation belt dynamics. Interplanetary shocks interaction with the Earth’s magnetosphere manifests many fundamental space physics phenomena including energetic particle acceleration. The mechanism of fast acceleration of energetic electrons in the radiation belt responding to interplanetary shock impacts consists of three contributing parts: (1) the initial adiabatic acceleration due to strong shock-related magnetic field compression; (2) followed by the drift-resonant acceleration with poloidal ULF waves excited at different L-shells; and (3) particle acceleration due to the quickly damping electric fields associated with ULF waves. Particles end up with a net acceleration because they gain more energy in the first half of this cycle than they lose in the second. The results reported in this paper cast a new light on understanding the acceleration of energetic particles in the Earth’s Van Allen radiation belt. The results of this study can likewise be applied to interplanetary shock interaction with other planets such as Mercury, Jupiter, Saturn, Uranus and Neptune, and other astrophysical objects with magnetic fields.     

Super solar particle event around AD775 was found

A rapid radiocarbon14C increase of 120/00in AD774–775 has been reported in cedar and oak tree rings.So far,the origin of the14C increase is still uncertain and the possible origin is either supernova or solar particle event.The most possible origin of14C increase is strong solar flares and Coronal Mass Ejections(CMEs)with strong particles emission.Comprehensive approaches to identify the strong historical solar particle events based on the rapid14C/10Be increase in tree/coral rings and ice cores,long duration strong auroras and geomagnetic storms are introduced.Evidence of the super auroras in AD775 was first found in a Chinese Chronicles Jiutangshu and it supports the views that the rapid14C increase and strong auroras around AD775 are most possibly caused by strong solar storms with intense particles emission.It was identified that the solar event around AD775 would be the strongest solar particle event in the past 11400 years.The discovery is significant for the research on the history of solar activities,space weather and forecast,radiation of solar energetic particles and protection.     

质子剂量微分谱预估空间辐射剂量

利用M on te C arlo方法结合小体积元人体模型对航天员空间质子辐射剂量进行估算。使用核磁共振全身扫描图像,通过识别组织器官,再利用参考人数据,建立由4mm×4mm×4mm小体积元组成的人体模型。该人体模型包括23种辐射敏感器官,并用查找表技术压缩模型数据。使用GEANT 4 M on te C arlo程序包,结合该模型,计算得到各个组织器官单能质子入射下的微分剂量估计谱库。对空间质子微分注量谱和微分剂量能谱积分,得到空间辐射剂量估计值。估算出1972年8月太阳质子事件的皮肤当量剂量为9 256 cSv,与文献值9 350 cSv相近,验证了算法的可行性。     

Wave acceleration of electrons in the Van Allen radiation belts

The Van Allen radiation belts are two regions encircling the Earth in which energetic charged particles are trapped inside the Earth's magnetic field. Their properties vary according to solar activity and they represent a hazard to satellites and humans in space. An important challenge has been to explain how the charged particles within these belts are accelerated to very high energies of several million electron volts. Here we show, on the basis of the analysis of a rare event where the outer radiation belt was depleted and then re-formed closer to the Earth, that the long established theory of acceleration by radial diffusion is inadequate; the electrons are accelerated more effectively by electromagnetic waves at frequencies of a few kilohertz. Wave acceleration can increase the electron flux by more than three orders of magnitude over the observed timescale of one to two days, more than sufficient to explain the new radiation belt. Wave acceleration could also be important for Jupiter, Saturn and other astrophysical objects with magnetic fields.     

Electron acceleration from contracting magnetic islands during reconnection

A long-standing problem in the study of space and astrophysical plasmas is to explain the production of energetic electrons as magnetic fields 'reconnect' and release energy. In the Earth's magnetosphere, electron energies reach hundreds of thousands of electron volts (refs 1-3), whereas the typical electron energies associated with large-scale reconnection-driven flows are just a few electron volts. Recent observations further suggest that these energetic particles are produced in the region where the magnetic field reconnects. In solar flares, upwards of 50 per cent of the energy released can appear as energetic electrons. Here we show that electrons gain kinetic energy by reflecting from the ends of the contracting 'magnetic islands' that form as reconnection proceeds. The mechanism is analogous to the increase of energy of a ball reflecting between two converging walls--the ball gains energy with each bounce. The repetitive interaction of electrons with many islands allows large numbers to be efficiently accelerated to high energy. The back pressure of the energetic electrons throttles reconnection so that the electron energy gain is a large fraction of the released magnetic energy. The resultant energy spectra of electrons take the form of power laws with spectral indices that match the magnetospheric observations.     

超短超强激光与等离子体相互作用中质子发射一些研究进展

超短超强激光与等离子体相互作用中得到的高能质子在质子成像、粒子加速、诊断超短超强激光与等离子体相互作用的物理过程、“快点火”和治疗癌症等方面有一定的应用。使得对超短超强激光与等离子体相互作用得到的高能质子的研究成为目前的研究热点。文章综述了产生质子的两种主要加速机制以及在不同实验条件下超短超强激光与等离子体相互作用过程中得到质子的能量、角分布、产额以及相关的原理。     

质子对碲锌镉辐照损伤的SRIM模拟

模拟计算质子对CdZnTe的辐照损伤. 先计算质子在CdZnTe中的电离损伤和位移损伤, 再计算不同能量和入射角的质子辐照CdZnTe产生的空位数, 最后计算不同能量和入射角的质子辐照不同厚度CdZnTe靶的溅射产额. 结果表明: 电离损伤远大于位移损伤; CdZnTe内因质子辐照产生的空位数随质子能量的增大而增加, 当质子入射角大于60°时, 产生的空位数明显减少; CdZnTe低于半导体硅和金刚石的抗辐照性能; 溅射产额与空位数相差较大, 溅射产额随质子能量的增大先增大后减小, 随质子入射角的增大而增大, 随CdZnTe靶厚度的增大整体趋于增大.     

地球磁场中任意投掷角的带电粒子运动轨迹

磁暴和亚暴过程中等离子体片带电粒子的注入严重影响了地球空间环境,导致环电流的增强或衰减,形成质子极光,影响中高层大气的物理化学过程。本研究利用UBK方法计算了穿越子夜(MLT=0)不同能量和投掷角的质子和电子漂移轨道,分析了粒子的来源区域和后续轨道特征。研究结果表明,穿过L=7的投掷角为90°的质子,能量低于~2keV时会逆时针绕地球作漂移运动,能量高于~4keV时则会顺时针绕地球作漂移运动。能量高于15keV的质子的漂移轨道形成闭合轨道。穿过L=7的投掷角为90°的电子均绕地球逆时针漂移,且能量高于5keV时形成闭合轨道。穿过L=4的质子,除了10keV左右的质子,轨道都呈现闭合状态,说明从等离子片来的10keV左右的质子可以更靠近地球;穿过L=4的电子都处在闭合轨道上。投掷角越小的质子越偏向于向晨侧运动,能量越高的质子受投掷角变化影响越小,投掷角的变化对电子的轨道几乎没有影响。Kp指数较大时,粒子的运动方向随能量变化不明显,但是轨道更难闭合,并更接近地球。     

太阳质子事件研究进展

太阳质子事件是很重要的太阳活动，从1956年开始人们对它进行了深入的趼究。概括太阳质子事件的研究进展：从质子事件的研究意义、不同时期的探测技术、质子在行星际介质空间的传播、质子事件的统计特征和相关性、质子峰值流量的分布、质子事件预报研究等几个方面对质子事件做了分析，有助于深入地了解太阳质子事件，从而更好地为空间天气预报服务。     

卫星太阳光压力矩计算中有效作用面积的计算

为了精确计算卫星在轨运行时所受的太阳光压力矩,给出了1种考虑太阳帆板与卫星体相互遮挡时太阳光压力矩的求取方法.将卫星体和太阳帆板组成的几何体进行投影变换后,判断其相互遮挡并采用凸多边形求交的算法求取太阳光压有效作用面积,从而计算太阳光压力矩.以某太阳同步轨道卫星为例进行计算,结果表明:当卫星体和太阳帆板的面积相比较小时,太阳光压力矩的求取可忽略卫星体以及卫星体对太阳帆板遮挡的影响.该方法同样可推广到考虑太阳帆板与卫星相互遮挡时气动力矩的求取.     

干涉光谱仪遥感探测的信噪比研究

干涉光谱仪进行空间目标探测时有很多影响因素。通过计算太阳对目标的表面辐射，利用大气传输模型分析软件——MODTRAN分析计算在可见光到近红外范围的天空漫反射辐射和背景辐射，给出探测器接收到的信号电子数。另外分析各种噪声源，给出主要噪声源的计算方法，并以电子数为基本单位表达各噪声的大小，从而推导出干涉光谱仪接收到的信噪比（以电子数为基本单位）的一般表达式。同时，分析各种因素对成像质量的影响，提出可行的方法改善成像质量。     

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。     

Electron dynamics in collisionless magnetic reconnection

Magnetic reconnection provides a physical mechanism for fast energy conversion from magnetic energy to plasma kinetic energy. It is closely associated with many explosive phenomena in space plasma, usually collisionless in character. For this reason, researchers have become more interested in collisionless magnetic reconnection. In this paper, the various roles of electron dynamics in collisionless magnetic reconnection are reviewed. First, at the ion inertial length scale, ions and electrons are decoupled. The resulting Hall effect determines the reconnection electric field. Moreover, electron motions determine the current system inside the reconnection plane and the electron density cavity along the separatrices. The current system in this plane produces an out-of-plane magnetic field. Second, at the electron inertial length scale, the anisotropy of electron pressure determines the magnitude of the reconnection electric field in this region. The production of energetic electrons, which is an important characteristic during magnetic reconnection, is accelerated by the reconnection electric field. In addition, the different topologies, temporal evolution and spatial distribution of the magnetic field affect the accelerating process of electrons and determine the final energy of the accelerated electrons. Third, we discuss results from simulations and spacecraft observations on the secondary magnetic islands produced due to secondary instabilities around the X point, and the associated energetic electrons. Furthermore, progress in laboratory plasma studies is also discussed in regard to electron dynamics during magnetic reconnection. Finally, some unresolved problems are presented.     

地球外太空的奥秘:一个巨大的动力辐射区域

2010年,作者在地球外太空发现一个以磁口(cusp)为中心的巨大的动力辐射区域.这个新辐射区域纵深可达10.5Re;在7-8Re高度上,其尺度在纬线和经线方向上可分别达到6Re和＞10Re;当人造卫星穿越该区域时,测得的电磁涨落强度与高能带电粒子强度都有数量级的增加.本文对此进行了综述分析,认为这是太空时代最关键和最...     

太阳同步轨道电子与质子对卫星的电离和非电离能损

空间辐射环境是飞行器寿命的主要限制因素之一。由于空间辐射环境的复杂性,以及飞行器在空间活动的轨道和设计寿命的不同,飞行器需要的抗辐射屏蔽的要求也不同。针对太阳同步轨道所处的空间辐射环境(由AE8和AP8提供该轨道的电子和质子能谱),采用Monte Carlo方法的PENELOPE和SHIELD软件包进行了模拟计算,研究了卫星所需的辐射屏蔽。根据模拟结果分析发现:在空间环境研究中,除了电离能损引起的总剂量外,由质子的非电离能损引起的位移损伤的影响不可忽略。质子和二次质子对电离能损、中子对非电离能损的贡献最大。     

Influence of low energy ballistic electron on the transmittance properties of Au/Si interface studied by ballistic-electron-emission microscope

Conclusions The electronic properties of Au/Si interface are investigated with a homemade ballistic-electron-emission microscope. The spatial distribution of Schottky barrier height is detected. Irreversible changes of ballistic transmittance of local interface with typical size of a few hundred of angstroms in diameter are observed by raising the tip voltage temporarily. Ballistic-electron-emission spectroscopy indicates that the electron transmission probabilities are reduced significantly inside the modified region, which is attributed to the Au-Si intermixing and other chemical reactions occurring at the interfacial layer stimulated by the injected energetic hot electrons.     

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.     

Energetic electrons associated with magnetic reconnection in the sheath of interplanetary coronal mass ejection

Magnetic reconnection is an important universal plasma dissipation process that converts magnetic energy into plasma thermal and kinetic energy,and simultaneously changes the magnetic field topology.In this paper,we report the first observation of energetic electrons associated with asymmetric reconnection in the sheath of an interplanetary coronal mass ejection.The magnetic field shear angle was about 151°,implying guide-field reconnection.The width of the exhaust was about 8×104 km.The reconnection rate was estimated as 0.044-0.08,which is consistent with fast reconnection theory and previous observations.We observed flux enhancements of energetic electrons with energy up to 400 keV in this reconnection exhaust.The region where ener- getic electron fluxes were enhanced is located at one pair of separatrices in the higher density hemisphere.We discuss these observation results,and compare with previous observations and recent kinetic simulations.