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We have performed a number of one-dimensional hybrid simulations (particle ions, massless electron fluid) of quasi-parallel collisionless shocks in order to investigate the injection and subsequent acceleration of part of the solar wind ions at the Earth’s bow shock. The shocks propagate into a medium containing magnetic fluctuations, which are initially superimposed on the background field, as well as generated or enhanced by the electromagnetic ion/ion beam instability between the solar wind and backstreaming ions. In order to study the mass (M) and charge (Q) dependence of the acceleration process He2+ is included self-consistently. The upstream differential intensity spectra of H+ and He2+ can be well represented by exponentials in energy. The e-folding energy Ec is a function of time: Ec increases with time. Furthermore the e-folding energy (normalized to the shock ramming energy Ep) increases with increasing Alfvén Mach number of the shock and with increasing fluctuation level of the initially superimposed turbulence. When backstreaming ions leave the shock after their first encounter they exhibit already a spectrum which extends to more than ten times the shock ramming energy and which is ordered in energy per charge. From the injection spectrum it is concluded that leakage of heated downstream particles does not contribute to ion injection. Acceleration models that permit thermal particles to scatter like the non-thermal population do not describe the correct physics. 相似文献
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采用日球子午面内的二维三分量MHD模型,研究瞬态激波的传播特性,着重分析日球 电流片（HCS）、日球等离子体片（HPS）和低速流结构对激波传播的影响．结果表明,HCS 和HPS对激波传播几乎没有影响,而跨越HCS和HPS的低速流则显著改变激波的传播特性. 低 速流对激波的反射,导致激波扰动源一侧的激波速度加快、强度增强,低速流对激波透射的 阻碍作用导致激波扰动源异侧的激波滞后、强度减弱,但激波阵面的纬度跨度有所加宽．在 激波穿越过后,低速流区朝激波传播方向弯曲并受到骚扰,使得激波下游出现复杂的扰动结 构;对于激波扰动源同侧的激波下游,反射波与该处等离子体的相互作用同样会导致较为复 杂的扰动出现. 相似文献
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A. V. Guglielmi L. E. Sobisevich A. L. Sobisevich I. P. Lavrov 《Izvestiya Physics of the Solid Earth》2014,50(4):501-507
The specific enhancement of ultra-low-frequency (ULF) electromagnetic oscillations a few hours prior to the strong earthquakes, which was previously mentioned in the literature, motivated us to search for the distinctive features of the mechanical (foreshock) activity of the Earth’s crust in the epicentral zones of the future earthquakes. Activation of the foreshocks three hours before the main shock is revealed, which is roughly similar to the enhancement of the specific electromagnetic ULF emission. It is hypothesized that the round-the-world seismic echo signals from the earthquakes, which form the peak of energy release 2 h 50 min before the main events, act as the triggers of the main shocks due to the cumulative action of the surface waves converging to the epicenter. It is established that the frequency of the fluctuations in the foreshock activity decreases at the final stages of the preparation of the main shocks, which probably testifies to the so-called mode softening at the approach of the failure point according to the catastrophe theory. 相似文献
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M. Gedalin 《Surveys in Geophysics》1997,18(6):541-566
Collisionless shocks are well-known to be very efficient energizers of ions. At the first step of energization relatively low energy suprathermal ion distributions are formed in the vicinity of the quasiperpendicular collisionless shock front during ion reflection and direct transmission. These distributions are formed promptly and at the scale of the shock width mainly due to the ion interaction with the quasistationary electromagnetic structure of the front itself. Their features are intimately related to the fine structure of the shock front in the sense that they depend not only on the bulk shock parameters, such as Mach number, but also on the details of the distribution of the fields, in particular, shock width. Therefore, studies of these distributions may provide valuable information about the shock structure itself. We review the observational data collected during in situ measurements (mainly at the Earth bow shock) and compare it to the numerical simulations and theoretical developments. The developed theory of the ion dynamics in the stationary shock front relates the ion reflection and heating to the insufficient deceleration of the ions in the ramp by the cross-shock potential, as compared to the expected downstream drift velocity, required by the Rankine-Hugoniot relations. As a result, the direct flow energy it transferred into the gyration energy, leading to the gyration of the ion distribution as a whole and enhanced spread in the velocity space, that is, effective collisionless heating. Anisotropy and nongyrotropy are typical features of ion distributions at both low and high-Mach number shocks, which is confirmed by observations. Time-dependent fields, which are not considered in the stationary shock model, are thought to provide subsequent smoothing and isotropization of the ion distributions. These processes occur at scales substantially larger than the shock width. 相似文献
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本文以几年来对海城地震宏观前兆资料系统整理和重点现象现场查实为基础,进一步研究了地震宏观前兆场的时空演变特征,各种宏观异常发展时间上的相关性,宏观异常的空间分布与活动断裂的关系。阐述了在地震短临孕育过程中,震前宏观异常所呈现的起伏性,空间分布上出现的密集条带、不均一和迁移性。在地震孕育的短临阶段应力的积累和加强随时间演化表现出起伏叠加,在空间上表现出孕震场内多点应力集中。并用震前宏观异常高潮期的起落对比,探索预报大地震临震的时间指标。用震前宏观异常在空间上分布的条带交叉和从外围向震中迁移的特点,探索了预报发震地点的可能性。最后对某些主要宏观异常的形成机制进行了初步讨论 相似文献
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It is well known that most MHD shocks observed within 1 AU are MHD fast shocks. Only a very limited number of MHD slow shocks are observed within 1 AU. In order to understand why there are only a few MHD slow shocks observed within 1 AU, we use a one-dimensional, time-dependent MHD code with an adaptive grid to study the generation and evolution of interplanetary slow shocks (ISS) in the solar wind. Results show that a negative, nearly square-wave perturbation will generate a pair of slow shocks (a forward and a reverse slow shock). In addition, the forward and the reverse slow shocks can pass through each other without destroying their characteristics, but the propagating speeds for both shocks are decreased. A positive, square-wave perturbation will generate both slow and fast shocks. When a forward slow shock (FSS) propagates behind a forward fast shock (FFS), the former experiences a decreasing Mach number. In addition, the FSS always disappears within a distance of 150R⊙ (where R⊙ is one solar radius) from the Sun when there is a forward fast shock (with Mach number \geq1.7) propagating in front of the FSS. In all tests that we have performed, we have not discovered that the FSS (or reverse slow shock) evolves into a FFS (or reverse fast shock). Thus, we do not confirm the FSS-FFS evolution as suggested by Whang (1987). 相似文献
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库玛断裂带强震活动与地震空区研究 总被引：12，自引：0，他引：12
库玛断裂带作为青藏高原内部的一条强地震活动带, 1900年以来发生过3次7级地震,其中2次7级大震前均出现5级以上地震的背景空区,表明背景空区对该带大震具有中长期预报意义。最近一次背景空区业已形成,并出现与之配套的孕震空区,其演化图像符合强震孕育模式。研究发现,库玛断裂带中段ML 3以上地震空区,对共和7级强震及周边200 km的强震有前兆意义。 相似文献
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A useful index for estimating the transit speeds was derived by analyzing interplanetary shock observations. This index is the ratio of the in situ local shock speed and the transit speed; it is 0.6–0.9 for most observed shocks. The local shock speed and the transit speed calculated for the results of the magnetohydrodynamic simulation show good agreement with the observations. The relation expressed by the index is well explained by a simplified propagation model assuming a blast wave. For several shocks the ratio is approximately 1.2, implying that these shocks accelerated during propagation in slow-speed solar wind. This ratio is similar to that for the background solar wind acceleration. 相似文献
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Gang Li 《中国科学:地球科学(英文版)》2017,60(8):1440-1465
In the solar system, our Sun is Nature’s most efficient particle accelerator. In large solar flares and fast coronal mass ejections (CMEs), protons and heavy ions can be accelerated to over ~GeV/nucleon. Large flares and fast CMEs often occur together. However there are clues that different acceleration mechanisms exist in these two processes. In solar flares, particles are accelerated at magnetic reconnection sites and stochastic acceleration likely dominates. In comparison, at CME-driven shocks, diffusive shock acceleration dominates. Besides solar flares and CMEs, which are transient events, acceleration of particles has also been observed in other places in the solar system, including the solar wind termination shock, planetary bow shocks, and shocks bounding the Corotation Interaction Regions (CIRs). Understanding how particles are accelerated in these places has been a central topic of space physics. However, because observations of energetic particles are often made at spacecraft near the Earth, propagation of energetic particles in the solar wind smears out many distinct features of the acceleration process. The propagation of a charged particle in the solar wind closely relates to the turbulent electric field and magnetic field of the solar wind through particle-wave interaction. A correct interpretation of the observations therefore requires a thorough understanding of the solar wind turbulence. Conversely, one can deduce properties of the solar wind turbulence from energetic particle observations. In this article I briefly review some of the current state of knowledge of particle acceleration and transport in the inner heliosphere and discuss a few topics which may bear the key features to further understand the problem of particle acceleration and transport. 相似文献
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本文利用邢台地震台网的地震目录资料,研究了邢台地区强震前小震的密集——平静特点及其空间分布的立体图象.研究结果表明: (1)1966年3月邢台地区发生的几个6级以上强震前小震均有密集——平静现象,但明显程度随时间减小.部份4.5级地震前小震也有密集——平静现象,但因出现在6级以上地震后的余震活动背景上,情况比较复杂.相对平静期的长度,密集期中最大地震的震级均与相应主震震级之间有一定关系.一般来讲,主震震级越大,平静期越长,密集期中最大地震震级也越大. (2)3月22日7.2级主震前,小震的密集——平静过程在空间上有清晰的物理图象.3月8日6.8级地震发生后,3月20日在其余震区的两个端部中介质强度较弱的南西端首先达到破裂强度,发生一系列中小地震,对应于主震前的密集期.3月21日至22日主震前小震明显减少,是主震前的相对平静期,而且小震有由南西端向北东方向迁移的趋势.显示震区应力场在迅速地改变,应力由南西端向北东端进一步集中,并促使22日在北东端尖端部位失稳而发生6.7级及7.2级主震.3月26日6.2级强震前小震的密集——平静过程在空间上也有类似清晰的物理图象. 此外,本文对大震前小震的密集——平静特点作初步的解释. 相似文献
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Pierre Lesaffre 《地球物理与天体物理流体动力学》2013,107(3):265-278
The author presents time-dependent analytical solutions of quasi-steady shocks with cooling, where quasi-steady shocks are objects composed of truncated steady-state models of shocks at any intermediate time. These solutions are compared to simulations with a hydrodynamical code and finally quasi-steady shocks are discussed as approximations to time-dependent shocks. Large departure of both the adiabatic and steady-state approximations from the quasi-steady solution emphasise the importance of the cooling history in determining the trajectory of a shock. 相似文献
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识别前震余震的单键群方法 总被引：3，自引：0，他引：3
本文提出一种从地震目录中识别强震的前震和余震并形成序列目标的新方法,即：以单键群（ＳＬＣ）分析方法为基础,定义在ＳＬＣ构架中,由于小于或等于特征键长的键所形成的许多链中,那些处在某个强震联通的链上的地震就与该强震构成一个地震序列;在此序列中,该强震为主震,之后的为余震,用此方法,可以按强震逐个识别其前震余震,并形成其序列目录。我们用它识别处理了海城７．４级和昆仑山－阿尔金山弧型顶部地区６．０级以上 相似文献