Thermodynamical Properties of the ICM from Hydrodynamical Simulations

Modern hydrodynamical simulations offer nowadays a powerful means to trace the evolution of the X-ray properties of the intra-cluster medium (ICM) during the cosmological history of the hierarchical build up of galaxy clusters. In this paper we review the current status of these simulations and how their predictions fare in reproducing the most recent X-ray observations of clusters. After briefly discussing the shortcomings of the self-similar model, based on assuming that gravity only drives the evolution of the ICM, we discuss how the processes of gas cooling and non-gravitational heating are expected to bring model predictions into better agreement with observational data. We then present results from the hydrodynamical simulations, performed by different groups, and how they compare with observational data. As terms of comparison, we use X-ray scaling relations between mass, luminosity, temperature and pressure, as well as the profiles of temperature and entropy. The results of this comparison can be summarised as follows: (a) simulations, which include gas cooling, star formation and supernova feedback, are generally successful in reproducing the X-ray properties of the ICM outside the core regions; (b) simulations generally fail in reproducing the observed “cool core” structure, in that they have serious difficulties in regulating overcooling, thereby producing steep negative central temperature profiles. This discrepancy calls for the need of introducing other physical processes, such as energy feedback from active galactic nuclei, which should compensate the radiative losses of the gas with high density, low entropy and short cooling time, which is observed to reside in the innermost regions of galaxy clusters.     

Synthesis of CME-Associated Moreton and EIT Wave Features from MHD Simulations

Soft X-ray (SXR) waves, EIT waves, and Hα Moreton waves are all associated with coronal mass ejections (CMEs). The knowledge of the characteristics about these waves is crucial for the understanding of CMEs, and hence for the space weather researches. MHD numerical simulation is performed, with the consideration of the quiet Sun atmosphere, to investigate the CME/flare processes. On the basis of the numerical results, SXR, EUV, and Hα images of the eruption are synthesized, where SXR waves, EIT waves, and Hα Moreton waves are identified. It confirms that the EIT waves, which border the expanding dimmming region, are produced by the successive opening (or stretching) of the closed magnetic field lines. Hα Moreton waves are found to propagate outward synchronously with the SXR waves, lagging behind the latter spatially by ～27 Mm in the simulated scenario. However, the EIT wave velocity is only a third of the Moreton wave velocity. The synthesized results also suggest that Hα± 0.45Å would be the best off-band for the detection of Hα Moreton waves.     

Solar filament eruptions and their physical role in triggering coronal mass ejections

Solar filament eruptions play a crucial role in triggering coronal mass ejections (CMEs). More than 80% of eruptions lead to a CME. This correlation has been studied extensively during the past solar cycles and the last long solar minimum. The statistics made on events occurring during the rising phase of the new solar cycle 24 is in agreement with this finding. Both filaments and CMEs have been related to twisted magnetic fields. Therefore, nearly all the MHD CME models include a twisted flux tube, called a flux rope. Either the flux rope is present long before the eruption, or it is built up by reconnection of a sheared arcade from the beginning of the eruption.     

对接综合试验台控制系统软件快速原型开发技术

对基于快速原型设计睁对接综合试验台控制系统软件开发进行了研究。介绍了根据系统方案进行的中央控制台软件设计和模型计算机软件开发等。给出了快速原型设计,以及包括接口设计、配置管理、文档管理等软件工程化管理等关键技术。     

Why should the latitude of the observer be considered when modeling gradual proton events? An insight using the concept of cobpoint

The shape of flux profiles of gradual solar energetic particle (SEP) events depends on several not well-understood factors, such as the strength of the associated shock, the relative position of the observer in space with respect to the traveling shock, the existence of a background seed particle population, the interplanetary conditions for particle transport, as well as the particle energy. Here, we focus on two of these factors: the influence of the shock strength and the relative position of the observer. We performed a 3D simulation of the propagation of a coronal/interplanetary CME-driven shock in the framework of ideal MHD modeling. We analyze the passage of this shock by nine spacecraft located at ∼0.4 AU (Mercury’s orbit) and at different longitudes and latitudes. We study the evolution of the plasma conditions in the shock front region magnetically connected to each spacecraft, that is the region of the shock front scanned by the “cobpoint” (Heras et al., 1995), as the shock propagates away from the Sun. Particularly, we discuss the influence of the latitude of the observer on the injection rate of shock-accelerated particles and, hence, on the resulting proton flux profiles to be detected by each spacecraft.     

Rayleigh问题的Monte Carlo直接模拟

利用流场直接模拟的Ｍｏｎｔｅ Ｃａｒｌｏ方法数值模拟了Ｒａｙｌｅｉｇｈ问题的流场，获得了相应的结果，结果与解析解及经验解吻合较好，ＤＳＭＣ方法避免了求解复杂的控制方程，在流动比较复杂的情形下，有很大的优越性，是研究稀薄气体流动的一种好方法。     

基于表面粘结损伤的复合固体推进剂细观损伤数值模拟

为更准确地模拟固体推进剂的细观损伤,研究复合固体推进剂的非线性力学性能,采用分子动力学方法对高填充比复合固体推进剂细观模型进行建模,验证了Surface-based cohesive方法的可行性,并替代经典粘结单元模拟了复合固体推进剂细观颗粒与基体之间界面损伤的产生和聚合.通过对比固体推进剂细观模型的计算结果,研究了复合固体推进剂颗粒粒径、位置的随机分布对固体推进剂细观损伤及宏观力学性能的影响.结果表明,采用Surface-based cohesive方法对固体推进剂细观模型较易进行有限元前处理,易收敛,计算结果比较合理.     

无人机飞行控制仿真系统研究

针对某型无人机的研制开发,提出了可行的仿真系统设计方案。首先设计全数字仿真验证飞行控制律的有效性,在此基础上,根据使用条件的差异,设计了两种相互关联的半物理仿真系统,即不带转台的半物理仿真以及带转台的半物理仿真,用来模拟无人机的飞行状况。最后给出了仿真的部分曲线。仿真结果表明,以上这种仿真系统可以对整个无人机飞控系统设计的合理性及有效性进行完备的验证,对同类飞行器仿真系统的研发具有一定的参考价值。     

基于复合模型及FSQP算法的发动机性能寻优控制试验

提出了一种在保证优化效果前提下提高发动机在线性能寻优实时性的方法,即一方面基于相似理论建立了适用于非加力状态的发动机复合稳态模型,在优化过程中替代原部件级模型以缩短优化计算时间,另一方面采用先进的可行性序列二次规划算法寻求全局最优解,以提高优化精度。最终实现了上述方案在最小油耗模式及最大推力模式下的数字仿真及半物理模拟验证,相比于传统的基于发动机部件级模型进行性能寻优控制,其优化精度相当,但优化实时性得到大幅度提高,从仿真结果可以看出上述方案的有效性及可行性。     

MHD code using multi graphical processing units: SMAUG+

This paper introduces the Sheffield Magnetohydrodynamics Algorithm Using GPUs (SMAUG+), an advanced numerical code for solving magnetohydrodynamic (MHD) problems, using multi-GPU systems. Multi-GPU systems facilitate the development of accelerated codes and enable us to investigate larger model sizes and/or more detailed computational domain resolutions. This is a significant advancement over the parent single-GPU MHD code, SMAUG (Griffiths et al., 2015). Here, we demonstrate the validity of the SMAUG?+?code, describe the parallelisation techniques and investigate performance benchmarks. The initial configuration of the Orszag-Tang vortex simulations are distributed among 4, 16, 64 and 100?GPUs. Furthermore, different simulation box resolutions are applied: $1000\times 1000\text{,}2044\times 2044\text{,}4000\times 4000$ and $8000\times 8000$. We also tested the code with the Brio-Wu shock tube simulations with model size of 800 employing up to 10?GPUs. Based on the test results, we observed speed ups and slow downs, depending on the granularity and the communication overhead of certain parallel tasks. The main aim of the code development is to provide massively parallel code without the memory limitation of a single GPU. By using our code, the applied model size could be significantly increased. We demonstrate that we are able to successfully compute numerically valid and large 2D MHD problems.