Orbit propagation around small bodies using spherical harmonic coefficients obtained from polyhedron shape models

P. Peñarroya, R. Paoli
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Abstract

Abstract Missions to asteroids have been the trend in space exploration for the last years. They provide information about the formation and evolution of the Solar System, contribute to direct planetary defense tasks, and could be potentially exploited for resource mining. Be their purpose as it may, the factor that all these mission types have in common is the challenging dynamical environment they have to deal with. The gravitational environment of a certain asteroid is most of the times not accurately known until very late mission phases when the spacecraft has already orbited the body for some time. Shape models help to estimate the gravitational potential with a density distribution assumption (usually constant value) and some optical measurements of the body. These measurements, unlike the ones needed for harmonic coefficient estimation, can be taken from well before arriving at the asteroid’s sphere of influence, which allows to obtain a better approximation of the gravitational dynamics much sooner. The disadvantage they pose is that obtaining acceleration values from these models implies a heavy computational burden on the on-board processing unit, which is very often too time-consuming for the mission profile. In this paper, the technique developed on [1] is used to create a validated Python-based tool that obtains spherical harmonic coefficients from the shape model of an asteroid or comet, given a certain density for the body. This validated software suite, called AstroHarm, is used to analyse the accuracy of the models obtained and the improvements in computational efficiency in a simulated spacecraft orbiting a small body. The results obtained are shown offering a qualitative comparison between different order spherical harmonic models and the original shape model. Finally, the creation of a catalogue for harmonics is proposed together with some thoughts on complex modelling using this tool.
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利用多面体形状模型得到的球谐系数进行小天体轨道传播
近年来,小行星任务一直是太空探索的趋势。它们提供了关于太阳系形成和演化的信息,有助于直接的行星防御任务,并可能被用于资源开采。不管它们的目的是什么,所有这些任务类型都有一个共同点,那就是它们必须应对具有挑战性的动态环境。在大多数情况下,直到任务的最后阶段,即航天器已经绕小行星运行了一段时间之后,人们才能准确地知道某颗小行星的引力环境。形状模型利用密度分布假设(通常为常数)和物体的一些光学测量来帮助估计重力势。与谐波系数估算所需的测量不同,这些测量可以在到达小行星的影响范围之前很久就进行,从而可以更快地获得引力动力学的更好近似值。它们的缺点是,从这些模型中获得加速度值意味着对机载处理单元的沉重计算负担,对于任务剖面来说,这通常过于耗时。本文使用[1]中开发的技术创建了一个经过验证的基于python的工具,该工具可以从给定一定密度的小行星或彗星的形状模型中获得球谐系数。这个经过验证的软件套件被称为AstroHarm,用于分析所获得模型的准确性,以及在模拟绕小天体运行的航天器中计算效率的改进。所得到的结果对不同阶的球谐模型和原形状模型进行了定性比较。最后,提出了谐波目录的创建,并提出了使用该工具进行复杂建模的一些想法。
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