Basic Physical Mechanism of Fast Reconnection Evolution in Space Plasmas

Large dissipative events, such as solar flares and geomagnetic substorms, may result from sudden onset of fast (explosive) magnetic reconnection. Hence, it is a long-standing problem to find the physical mechanism that makes magnetic reconnection explosive; in particular, how can the fast magnetic reconnection explosively evolve in space plasmas? In this respect, we have proposed the spontaneous fast reconnection model as a nonlinear instability that grows by the positive feedback between plasma microphysics (anomalous resistivity) and macrophysics (global reconnection flow). On the basis of MHD simulations, we demonstrate for a variety of physical situations that the fast reconnection mechanism involving slow shocks in fact evolves explosively as a nonlinear instability and is sustained quasi-steadily on the nonlinear saturation phase. Also, distinct plasma processes, such as large-scale plasmoid propagation, magnetic loop development and loop-top heating, and asymmetric fast reconnection evolution, directly result from the spontaneous fast reconnection model. Obviously, MHD simulations are very useful in understanding the basic physics of explosive fast reconnection evolution in space plasmas. However, they cannot treat the details of microphysics near an X neutral point, which should be precisely studied in the coming 21st century.     

水下强声波脉冲引发的空化气泡运动和声辐射

通过建立由等离子体声源、PCB压力传感器和高速相机等构成的实验测量系统,研究了强声波脉冲引发的空化气泡运动和二次声辐射。通过实验,观察到了强声波脉冲特有的波形结构,空化气泡的成长、膨胀和坍缩过程以及气泡坍缩时辐射的声信号。其次,利用Gilmore方程和Bernoulli方程,从理论上对空化气泡的运动和声辐射进行了数值模拟和分析。研究结果表明：（1）在强声波脉冲正压区的作用下,空化气泡将受到压缩并围绕＂准平衡态半径＂振荡;在强声波脉冲负压区的作用下,空化气泡将出现膨胀、坍缩和回弹的物理过程。（2）空化气泡坍缩时周期性辐射的声脉冲持续时间极短,具有＂冲击波＂的特点。     

Recent Advances in Understanding Particle Acceleration Processes in Solar Flares

We review basic theoretical concepts in particle acceleration, with particular emphasis on processes likely to occur in regions of magnetic reconnection. Several new developments are discussed, including detailed studies of reconnection in three-dimensional magnetic field configurations (e.g., current sheets, collapsing traps, separatrix regions) and stochastic acceleration in a turbulent environment. Fluid, test-particle, and particle-in-cell approaches are used and results compared. While these studies show considerable promise in accounting for the various observational manifestations of solar flares, they are limited by a number of factors, mostly relating to available computational power. Not the least of these issues is the need to explicitly incorporate the electrodynamic feedback of the accelerated particles themselves on the environment in which they are accelerated. A brief prognosis for future advancement is offered.     

Energy Release and Particle Acceleration in Flares: Summary and Future Prospects

RHESSI measurements relevant to the fundamental processes of energy release and particle acceleration in flares are summarized. RHESSI??s precise measurements of hard X-ray continuum spectra enable model-independent deconvolution to obtain the parent electron spectrum. Taking into account the effects of albedo, these show that the low energy cut-off to the electron power-law spectrum is typically ?tens of keV, confirming that the accelerated electrons contain a large fraction of the energy released in flares. RHESSI has detected a high coronal hard X-ray source that is filled with accelerated electrons whose energy density is comparable to the magnetic-field energy density. This suggests an efficient conversion of energy, previously stored in the magnetic field, into the bulk acceleration of electrons. A new, collisionless (Hall) magnetic reconnection process has been identified through theory and simulations, and directly observed in space and in the laboratory; it should occur in the solar corona as well, with a reconnection rate fast enough for the energy release in flares. The reconnection process could result in the formation of multiple elongated magnetic islands, that then collapse to bulk-accelerate the electrons, rapidly enough to produce the observed hard X-ray emissions. RHESSI??s pioneering ??-ray line imaging of energetic ions, revealing footpoints straddling a flare loop arcade, has provided strong evidence that ion acceleration is also related to magnetic reconnection. Flare particle acceleration is shown to have a close relationship to impulsive Solar Energetic Particle (SEP) events observed in the interplanetary medium, and also to both fast coronal mass ejections and gradual SEP events. New instrumentation to provide the high sensitivity and wide dynamic range hard X-ray and ??-ray measurements, plus energetic neutral atom (ENA) imaging of SEPs above ??2 R_??, will enable the next great leap forward in understanding particle acceleration and energy release is large solar eruptions??solar flares and associated fast coronal mass ejections (CMEs).     

FUV and X-Ray Absorption in the Warm-Hot Intergalactic Medium

The Warm-Hot Intergalactic Medium (WHIM) arises from shock-heated gas collapsing in large-scale filaments and probably harbours a substantial fraction of the baryons in the local Universe. Absorption-line measurements in the ultraviolet (UV) and in the X-ray band currently represent the best method to study the WHIM at low redshifts. We here describe the physical properties of the WHIM and the concepts behind WHIM absorption line measurements of H i and high ions such as O vi, O vii, and O viii in the far-ultraviolet and X-ray band. We review results of recent WHIM absorption line studies carried out with UV and X-ray satellites such as FUSE, HST, Chandra, and XMM-Newton and discuss their implications for our knowledge of the WHIM.     

Observations of loops and prominences

We review recent observations by the Yohkoh-SXT in collaboration with other spacecraft and ground-based observatories of coronal loops and prominences. These new results point to problems that SoHO will be able to address. With a unique combination of rapid-cadence digital imaging (32 s full-disk and 2 s partial-frame images), high spatial resolution (2.5 arcsec pixels), high sensitivity (EM 10⁴² cm^–3), a low-scatter mirror, and large dynamic range, SXT can observe a vast range of targets on the Sun. Over the first 21 months of Yohkoh operations, SXT has taken over one million images of the corona and so is building up an invaluable long-term database on the large-scale corona and loop geometry. The most striking thing about the SXT images is the range of loop sizes and shapes. The active regions are a bright tangle of magnetic field lines, surrounded by a network of large-scale quiet-Sun loops stretching over distances in excess of 10⁵ km. The cross-section of most loops seems to be constant. Loops displaying significant increase in the ratio of the footpoint to loop-top diameter () are the exception, not the rule, implying the presence of widespread currents in the corona.All magnetic structures show changes. Time scales range from seconds to months. The question of how these structures are formed, become filled with hot plasma, and are maintained is still open. While we see the propagation of brightenings along the length of active-region loops and in X-ray jets with velocities of several hundred km/s, much higher velocities are seen in the quiet Sun. In XBP flares, for example, velocities of over 1000 km/s are common. Active-region loops seem to be in constant motion, moving slowly outward, carrying plasma with them. During flares, loops often produce localized brightenings at the base and later at the apex of the loop. Quiescent filaments and prominences have been observed regularly. Their coronal manifestation seems to be an extended arcade of loops overlying the filament. Reliable alignment of the ground-based data with the X-ray images make it possible to make a detailed intercomparison of the hot and cold plasma structures over extended periods. Hence we are able to follow the long-term evolution of these structures and see how they become destabilized and erupt.     

基于贝叶斯优化的磁光阱多参数自主优化系统

磁光阱是一种冷却陷俘原子的装置，磁光阱实验参数的优化是冷原子实验中基础且重要的工作，人工手动优化参数需耗费大量时间，且很难确保最终参数是全局最优的。基于贝叶斯优化的机器学习方法是一种对目标表达式未知、非凸、多峰的量子物理系统进行参数优化的有效方案，该过程通常远快于人工手动调节，且有更大概率找到全局最优值。提出了一种基于贝叶斯优化方法的冷原子多参数自主实时优化实验方案，该方案通过成本函数构造、控制程序编写、贝叶斯算法优化等形成一个可自主优化的闭环系统。实验结果表明，经过约30 min的迭代优化，所提方案可有效完成磁光阱系统的多参数优化，并得到最优的实验结果；所提方案验证了贝叶斯优化方法在多参数物理系统中应用的可行性，通过改进成本函数，还可应用于其他的复杂多参数实验物理系统最优参数快速确定。     

Magnetic Fields in Supernova Remnants and Pulsar-Wind Nebulae

We review the observations of supernova remnants (SNRs) and pulsar-wind nebulae (PWNe) that give information on the strength and orientation of magnetic fields. Radio polarimetry gives the degree of order of magnetic fields, and the orientation of the ordered component. Many young shell supernova remnants show evidence for synchrotron X-ray emission. The spatial analysis of this emission suggests that magnetic fields are amplified by one to two orders of magnitude in strong shocks. Detection of several remnants in TeV gamma rays implies a lower limit on the magnetic-field strength (or a measurement, if the emission process is inverse-Compton upscattering of cosmic microwave background photons). Upper limits to GeV emission similarly provide lower limits on magnetic-field strengths. In the historical shell remnants, lower limits on B range from 25 to 1000?μG. Two remnants show variability of synchrotron X-ray emission with a timescale of years. If this timescale is the electron-acceleration or radiative loss timescale, magnetic fields of order 1?mG are also implied. In pulsar-wind nebulae, equipartition arguments and dynamical modeling can be used to infer magnetic-field strengths anywhere from ～5?μG to 1?mG. Polarized fractions are considerably higher than in SNRs, ranging to 50 or 60% in some cases; magnetic-field geometries often suggest a toroidal structure around the pulsar, but this is not universal. Viewing-angle effects undoubtedly play a role. MHD models of radio emission in shell SNRs show that different orientations of upstream magnetic field, and different assumptions about electron acceleration, predict different radio morphology. In the remnant of SN 1006, such comparisons imply a magnetic-field orientation connecting the bright limbs, with a substantial density gradient across the remnant.     

Theories of magnetospheres around accreting compact objects

A wide class of galactic X-ray sources are believed to be binary systems where mass is flowing from a normal star to a companion that is a compact object, such as a neutron star. The strong magnetic fields of the compact object create a magnetosphere around it. We review the theoretical models developed to describe the properties of magnetospheres in such accreting binary systems. The size of the magnetosphere can be estimated from pressure balance arguments and is found to be small compared to the over-all size of the accretion region but large compared to the compact object if the latter is a neutron star. In the early models the magnetosphere was assumed to have open funnels in the polar regions, through which accreting plasma could pour in. Later, magnetically closed models were developed, with plasma entry made possible by instabilities at the magnetosphere boundary. The theory of plasma flow inside the magnetosphere has been formulated in analogy to a stellar wind with reversed flow; a complicating factor is the instability of the Alfvén critical point for inflow. In the case of accretion via a well-defined disk, new problems of magnetospheric structure appear, in particular the question to what extent and by what process the magnetic fields from the compact object can penetrate into the accretion disk. Since the X-ray emission is powered by the gravitational energy released in the accretion process, mass transfer into the magnetosphere is of fundamental importance; the various proposed mechanisms are critically examined.Proceedings of the NASA/JPL Workshop on the Physics of Planetary and Astrophysical Magnetospheres.     

Collapsing losses of peak signal integrators

Collapsing losses are computed for systems in which the peak return of K samples of noise plus one sample of signal-plus-noise are integrated over N looks. The statistical approach, collapsing losses, and an application are described. The peak integrator is found to have substantially lower collapsing losses than conventional systems in which the average, not the peak, is integrated     

实用化光力加速度计中单微球重复起支技术

针对光力加速度计的小型化应用，设计并制作了一种基于V型槽的片上光纤光阱，并采用机械振动方法实现了单微球重复起支。理论研究了利用机械振动方法实现微球起支、捕获的动力学过程。结果表明，只有当微球脱离捕获室底面的初始速度满足一定范围时才能稳定捕获，该初始速度范围与捕获室的几何参数有关。提出了利用两光纤中相向传播光的耦合功率监测微球捕获状态的方法，并通过实验完成了微球起支过程的自动控制，实现了单微球的重复起支与捕获。该片上光纤光阱制备方法和单微球重复起支技术可推动光力加速度计的实用化进程。     

实用化光力加速度计中单微球重复起支技术

针对光力加速度计的小型化应用,设计并制作了一种基于V型槽的片上光纤光阱,并采用机械振动方法实现了单微球重复起支。理论研究了利用机械振动方法实现微球起支、捕获的动力学过程。结果表明,只有当微球脱离捕获室底面的初始速度满足一定范围时才能稳定捕获,该初始速度范围与捕获室的几何参数有关。提出了利用两光纤中相向传播光的耦合功率监测微球捕获状态的方法,并通过实验完成了微球起支过程的自动控制,实现了单微球的重复起支与捕获。该片上光纤光阱制备方法和单微球重复起支技术可推动光力加速度计的实用化进程。     

薄膜充气梁失稳载荷研究

针对薄膜充气梁在弯曲载荷下的失稳载荷问题,进行了理论及试验研究,得到充气模型失稳载荷的理论值和试验值,两者对比显示试验值高于理论值1.56倍以上,为在使用过程中充分利用充气模型的承载能力提供了有效的数据。     

民用飞机翼身对接斜撑板结构分析

斜撑板结构可以充分发挥分散载荷和降低区域应力水平的作用。对不同机型的斜撑板结构的传力特性进行分析,总结斜撑板结构的设计要点。并以某机型选用斜撑板结构的设计为例,提出一种斜撑板结构的改进方案(斜撑板侧边和后梁框刚性连接、下边和对接带板充分连接),并与其他两种设计方案进行对比分析。结果表明:改进方案的斜撑板结构翼上区和舱上区的剪应力分别降低了19%和23%,后梁框的集中载荷降低了67%,结构效率更高、稳定性更好。     

Magnetic alignment and counter-alignment in binary X-ray pulsars

The magnetic torque exerted on a binary X-ray pulsar acts to decrease the angle between the dipole and spin axes during braking episodes, but to increase it whenever spinup occurs. The likely effect on the X-ray pulse profiles is considered.     

A magnetic explanation for the rapid burster

The observations of X-ray Type II bursts from the low-mass X-ray binary MXB 1730-335 can be explained by a particular form of magnetic gating in the presence of steady external accretion. The requirements are a strong magnetic field of the neutron star (7×10¹¹–2×10¹² gauss at the surface), rotational symmetry and alignment of the field axis with the axis of a steadily accreting disk to within 6°.     

泡沫夹层结构复合材料准静态压痕实验

研究了两种芯材高度的泡沫夹层结构复合材料在准静态压痕力下的损伤过程与形式,通过控制压头位移得到位移与接触力的关系曲线以及不同位移下的损伤形貌,比较了两种芯材的损伤过程.结果表明:损伤过程为泡沫塌陷、泡沫芯材出现裂纹、夹层板上蒙皮分层和芯材与下蒙皮脱粘;损伤形式为:厚芯材时裂纹与泡沫厚度方向成±45.,薄芯材时裂纹与泡沫厚度方向成90°.     

Microstructure and Magnetic Anisotropy of FeCoNbB Films

Effect of Nb contents on microstructure and magnetic properties of FeCoNbB films has been studied. X-ray diffraction (XRD) analysis reveals that Nb plays a role in refining grain and in facilitating formation of amorphous structure. When Nb content is more than 8 at%, the films transform from crystalline to amorphous structure, accompanied by variations in magnetic properties. An unusual out-of-plane anisotropy component is consequently observed. It can be suggested that the anisotropy induced by increasing Nb contents be attributed to stress-related magnetoelastic anisotropy. The undesirable anisotropy is greatly reduced by thermal annealing, reducing film thicknesses or applying an external magnetic field together with Si addition.     

30CrMnSiNi2A超高强度钢真空电子束焊接工艺应用研究

针对锁底对接形式的30CrMnSiNi2A超高强度钢进行了真空电子束焊接工艺分析与讨论,借助金相分析、显微硬度、扫描电镜等测试方法对焊缝形貌、组织和性能进行了研究,并分析了常见缺陷的种类和防止措施。试验结果表明,在合适的电子束焊接参数下可以获得较为理想的30CrMnSiNi2A超高强度钢焊缝形貌,且具有较好的综合力学性能,焊缝经目视检查、X射线探伤和磁粉探伤,达到I级焊缝要求,并将此焊接工艺成功地应用于飞机机体产品的焊接。     

Implications of X-ray Observations for Electron Acceleration and Propagation in Solar Flares

High-energy X-rays and ??-rays from solar flares were discovered just over fifty years ago. Since that time, the standard for the interpretation of spatially integrated flare X-ray spectra at energies above several tens of keV has been the collisional thick-target model. After the launch of the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) in early 2002, X-ray spectra and images have been of sufficient quality to allow a greater focus on the energetic electrons responsible for the X-ray emission, including their origin and their interactions with the flare plasma and magnetic field. The result has been new insights into the flaring process, as well as more quantitative models for both electron acceleration and propagation, and for the flare environment with which the electrons interact. In this article we review our current understanding of electron acceleration, energy loss, and propagation in flares. Implications of these new results for the collisional thick-target model, for general flare models, and for future flare studies are discussed.