Methodological Characterization and Computational Codes in the Simulation of Interacting Galaxies

Eduardo Teófilo-Salvador, P. Ambrocio-Cruz, Margarita Rosado-Solís
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Abstract

Currently, technological development has exponentially fostered a growing collection of dispersed and diversified information. In the case of galaxy interaction studies, it is important to identify and recognize the parameters in the process, the tools and the computational codes available to select the appropriate one in depending on the availability of data. The objective was to characterize the parameters, techniques and methods developed, as well as the computational codes for numerical simulation. From the bibliography, it was reviewed how various authors have studied the interaction, presence of gas and star formation, then the review of computer codes with the requirements and benefits, to analyze and compare the initial and boundary conditions. With images, the CNN method programmed in python was applied to identify the differences and their possible accuracy. SPH systems have more robust algorithms, invariance, simplicity in implementation, flexible geometries, but do not parameterize artificial viscosities, discontinuous solutions and instabilities. In the case of AMR there is no artificial viscosity, resolution of discontinuities, suppression of instabilities, but with complex implementation, mesh details, resolution problems and they are not scalable. It is necessary to use indirect methods to infer some properties or perform preliminary iterations. The availability of observable data governs the behavior of possible numerical simulations, in addition to having tools such as a supercomputer, generating errors that can be adjusted, compared or verified, according to the techniques and methods shown in this study, in addition to the fact that codes that are not so well known and used stand out as those that are currently more applied.
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相互作用星系模拟中的方法表征和计算代码
目前,技术发展以指数方式促进了分散和多样化信息的收集。在星系相互作用研究的情况下,重要的是确定和识别过程中的参数,工具和计算代码,以根据数据的可用性选择适当的一个。目的是描述所开发的参数、技术和方法,以及数值模拟的计算代码。从参考书目中,回顾了不同作者如何研究相互作用、气体的存在和恒星的形成,然后回顾了计算机代码的要求和优点,分析和比较了初始条件和边界条件。对于图像,使用python编程的CNN方法来识别差异及其可能的准确性。SPH系统具有更强的算法鲁棒性、不变性、实现简单、几何形状灵活,但不能参数化人工粘度、不连续解和不稳定性。在AMR的情况下,没有人工粘度,不连续性的分辨率,不稳定性的抑制,但复杂的实现,网格细节,分辨率问题,它们是不可扩展的。有必要使用间接方法来推断某些属性或执行初步迭代。可观测数据的可用性决定了可能的数值模拟的行为,除了拥有超级计算机等工具,根据本研究中显示的技术和方法,产生可以调整、比较或验证的错误,以及那些不太为人所知和使用的代码比目前更广泛应用的代码更突出这一事实。
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