We discuss the dynamics of asteroids possessing perihelion distances shorter than 0.15 au because this value is close to the perihelion distance of (3200) Phaethon (0.14 au). A well-elaborated force model is necessary to describe the motion of the discussed objects. In this study, we examined the following factors affecting an asteroid's motion: perturbations from all major planets and those from Pluto, Moon, Ceres, Pallas, and Vesta, Sun's and Jupiter's oblateness, relativistic effects of the Sun and all major planets (as well as Pluto and the Moon), solar radiation pressure, and the Yarkovsky effect. All five methods are based on the analysis of (O–C) residuals (differences between the observed and calculated coordinate values), the size of the initial confidence region, and the orbital evolution. This demonstrates that there exists a close correlation between all five methods. We arranged the perturbing forces in accordance with their power as follows (the most powerful first): perturbations from major planets, from the Moon, the relativistic effects of the Sun, and the Sun's oblateness. The relativistic effects of the other bodies were negligible. In addition, we paid special attention to the Yarkovsky effect. Our results showed that it significantly affected the asteroid motion. However, currently, we cannot confidently and precisely isolate its contribution to the full force model because of the insufficient precision of its parameter definition. The obtained results could be used to study the dynamics of near-Sun asteroids, which we illustrate by exploring the orbital evolution of the (3200) Phaethon asteroid.

我们讨论了近日距离小于0.15 au的小行星的动力学，因为该值接近（3200）Phaethon（0.14 au）的近日距离。精心设计的力模型对于描述所讨论对象的运动是必要的。在这项研究中，我们研究了以下影响小行星运动的因素：所有主要行星的扰动以及冥王星，月球，谷神星，帕拉斯和维斯塔的扰动，太阳和木星的扁率，太阳和所有主要行星的相对论效应（以及如冥王星和月球），太阳辐射压力和雅尔科夫斯基效应。所有这五种方法都基于对（OC）残差（观测值与计算出的坐标值之间的差异），初始置信区域的大小以及轨道演化的分析。这表明这五种方法之间存在密切的相关性。我们按照它们的力量来排列扰动力，如下（最强大的第一项）：主要行星，月球的扰动，太阳的相对论效应以及太阳的扁率。其他机构的相对论影响可忽略不计。此外，我们特别注意了Yarkovsky效应。我们的结果表明，它显着影响了小行星的运动。但是，由于其参数定义的精度不足，目前我们无法自信，准确地分离出其对全力模型的贡献。所得结果可用于研究近太阳小行星的动力学，我们将通过探索（3200）费森小行星的轨道演化来说明这一点。