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1.
Particle Acceleration at Interplanetary Shocks   总被引:1,自引:0,他引:1  
This paper briefly reviews proton acceleration at interplanetary shocks. This is key to describing the acceleration of heavy ions at interplanetary shocks because wave excitation—and hence particle scattering—at oblique shocks is controlled by the protons and not the heavy ions. Heavy ions behave as test particles, and their acceleration characteristics are controlled by the properties of proton-excited turbulence. As a result, the resonance condition for heavy ions introduces distinctly different signatures in abundance, spectra, and intensity profiles, depending on ion mass and charge. Self-consistent models of heavy-ion acceleration and the resulting fractionation are discussed. This includes discussion of the injection problem and the acceleration characteristics of quasi-parallel and quasi-perpendicular shocks.  相似文献   

2.
从2005年上半年显示的种种迹象表明,全球航空运输业已经走上了复苏的轨道,但进入下半年后却意想不到地遭到接二连三的打击。首先,国际油价的一路飙升促使航空公司的运营成本节节升高,吞噬了航空公司的利润空间,尽管今年航班的客流量有较大幅度的上升,但客票收入的增长远不足以弥补成本的增加。业内人士分析,如果油价超过每桶60美元以后,收入增长将完全被燃油成本的上升所抵消,更何况现在的油价已经冲到了每桶近70美元,有人预计全球航空运输业今年的亏损将可能达到100亿美元。  相似文献   

3.
This paper reviews selected topics in cosmic-ray transport in the heliosphere, as well as recent insights on the interaction of cosmic rays with shocks. Topics include: (a) recent observations suggesting very long inferred scattering mean-free paths of cosmic rays, (b) recent insights into the diffusion of cosmic rays normal to a magnetic field, (c) the physics of super-diffusion and sub-diffusion, and (e) the interaction of cosmic rays with shocks moving through large-scale irregular magnetic fields.  相似文献   

4.
Shocks in collisionless plasmas require dissipation mechanisms which couple fields and particles at scales much less than the conventional collisional mean free path. For quasi-parallel geometries, where the upstream magnetic field makes a small angle to the shock normal direction, wave-particle coupling produces a broad transition zone with large amplitude, nonlinear magnetic pulsations playing an important role. At high Mach numbers, ion reflection and acceleration are dominant processes which control the structure and dissipation at the shock. Accelerated particles produce a precursor, or foreshock, characterized by low frequency magnetic waves which are convected by the plasma flow into the shock transition zone. The interplay between energetic particles, waves, ion reflection and acceleration leads to a complicated interdependent system. This review discusses the spacecraft observations which have motivated the current view of the high Mach number quasi-parallel shock, and the theories and simulation studies which have led to a better understanding of the microphysics on which the quasi-parallel shock depends.  相似文献   

5.
Shock waves originating from hypersonic projectiles flown in ballistic ranges and subsequently reflected from the range walls have been found to produce undesirable effects on the measurements of projectile wakes. This paper reports on the mechanisms through which reflected shock waves perturb the wake, the design, and installation of full-scale fiberglas wedge shock attenuation treatments, the design of equipment for minimum shock reflection, and the results of measurements of the performance of the treatment.  相似文献   

6.
将无网格自适应算法发展用于求解存在运动激波的非定常流动问题。为了降低初始布点要求,同时提高对运动激波的分辨率,提出了一种结合点云加密和点云粗化的动态点云技术。采用该技术,在非定常计算的每一个时间步,首先通过基于压强梯度的流场探针识别出激波所在位置,然后对激波附近点云进行加密,从而提高对激波的分辨率,同时对远离激波的点云进行粗化,尽可能减少冗余节点,提高计算效率。采用所提出的无网格自适应算法求解了N-S方程,首先对一维运动激波问题进行了数值模拟,通过将数值模拟结果与精确解比较,验证了所提算法求解存在运动激波的非定常流动的可行性,在此基础上,将方法推广用于二维非定常流动问题的求解,分别对瞬时激波碰撞圆柱以及双弧翼型激波振荡流动进行了数值模拟,计算结果表明,方法可以显著提高对激波的分辨率,同时相对于直接采用较密布点的非自适应算法,自适应算法在计算效率上具有优势。  相似文献   

7.
Electrons with near-relativistic (E≳30 keV, NrR) and relativistic (E≳0.3 MeV) energies are often observed as discrete events in the inner heliosphere following solar transient activity. Several acceleration mechanisms have been proposed for the production of those electrons. One candidate is acceleration at MHD shocks driven by coronal mass ejections (CMEs) with speeds ≳1000 km s−1. Many NrR electron events are temporally associated only with flares while others are associated with flares as well as with CMEs or with radio type II shock waves. Since CME onsets and associated flares are roughly simultaneous, distinguishing the sources of electron events is a serious challenge. On a phenomenological basis two classes of solar electron events were known several decades ago, but recent observations have presented a more complex picture. We review early and recent observational results to deduce different electron event classes and their viable acceleration mechanisms, defined broadly as shocks versus flares. The NrR and relativistic electrons are treated separately. Topics covered are: solar electron injection delays from flare impulsive phases; comparisons of electron intensities and spectra with flares, CMEs and accompanying solar energetic proton (SEP) events; multiple spacecraft observations; two-phase electron events; coronal flares; shock-associated (SA) events; electron spectral invariance; and solar electron intensity size distributions. This evidence suggests that CME-driven shocks are statistically the dominant acceleration mechanism of relativistic events, but most NrR electron events result from flares. Determining the solar origin of a given NrR or relativistic electron event remains a difficult proposition, and suggestions for future work are given.  相似文献   

8.
本文采用隐式CSCM格式,通过数值求解NS方程,对平板上二维超声速主流中横向喷流流场进行了数值模拟,并与实验和其它计算结果进行了分析比较,结果令人满意。  相似文献   

9.
Collisionless shocks are loosely defined as shocks where the transition between pre-and post-shock states happens on a length scale much shorter than the collisional mean free path. In the absence of collision to enforce thermal equilibrium post-shock, electrons and ions need not have the same temperatures. While the acceleration of electrons for injection into shock acceleration processes to produce cosmic rays has received considerable attention, the related problem of the shock heating of quasi-thermal electrons has been relatively neglected. In this paper we review the state of our knowledge of electron heating in astrophysical shocks, mainly associated with supernova remnants (SNRs), shocks in the solar wind associated with the terrestrial and Saturnian bowshocks, and galaxy cluster shocks. The solar wind and SNR samples indicate that the ratio of electron temperature, (T e ) to ion temperature (T p ) declining with increasing shock speed or Alfvén Mach number. We discuss the extent to which such behavior can be understood on the basis of waves generated by cosmic rays in a shock precursor, which then subsequently damp by heating electrons, and speculate that a similar explanation may work for both solar wind and SNR shocks.  相似文献   

10.
We present a brief introduction to the essential physics of coronal mass ejections as well as a review of theory and models of CME initiation, solar energetic particle (SEP) acceleration, and shock propagation. A brief review of the history of CME models demonstrates steady progress toward an understanding of CME initiation, but it is clear that the question of what initiates CMEs has still not been solved. For illustration, we focus on the flux cancellation model and the breakout model. We contrast the similarities and differences between these models, and we examine how their essential features compare with observations. We review the generation of shocks by CMEs. We also outline the theoretical ideas behind the origin of a gradual SEP event at the evolving CME-driven coronal/interplanetary shock and the origin of “impulsive” SEP events at flare sites of magnetic reconnection below CMEs. We argue that future developments in models require focused study of “campaign events” to best utilize the wealth of available CME and SEP observations.  相似文献   

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