论文标题
主要带的新的多部分碰撞模型：对近地小行星的贡献
New multi-part collisional model of the main belt: The contribution to near-Earth asteroids
论文作者
论文摘要
目标。我们开发了主要小行星带（MB）的六部分碰撞进化模型，并使用它来研究MB不同区域对近地球小行星（NEAS）的贡献。方法。我们构建了一个名为ACDC的统计代码，该代码模拟了MB的碰撞演化分为六个区域（即内部，中，原始，外部，外部，Cybele和高倾斜带），根据那里的主要共振位置（$ν_{6}} $，3：1J，3：1J，5：2J，5：2J，7：3J和2：3J和2：3J和2：1J）。我们将Yarkovsky效应和上述共振视为从MB不同地区去除小行星并将其交付到NEA地区的主要机制。我们通过考虑NEA人群中的共振和平均动力学时间尺度来计算来自不同来源区域的NEA的演变。结果。我们的模型与与MB相关的主要观察性约束一致，例如MB不同区域的大小分布和大型小行星家族的数量。它还能够以H <16的速度复制观察到的NEAS，并同意H <20的最新估计，但偏离了较小的尺寸。我们发现大多数消息来源对NEAS做出了重大贡献。但是，内部和中部带是最重要的NEAS来源，然后是外带。原始地区和赛贝尔地区的贡献很小。高倾斜带仅是实际观察到的NEAS的一部分的来源，因为该区域中存在动态过程，使小行星能够增加和减少其倾斜度。
Aims. We developed a six-part collisional evolution model of the main asteroid belt (MB) and used it to study the contribution of the different regions of the MB to the near-earth asteroids (NEAs). Methods. We built a statistical code called ACDC that simulates the collisional evolution of the MB split into six regions (namely Inner, Middle, Pristine, Outer, Cybele and High-Inclination belts) according to the positions of the major resonances present there ($ν_{6}$, 3:1J, 5:2J, 7:3J and 2:1J). We consider the Yarkovsky effect and the mentioned resonances as the main mechanism that removes asteroids from the different regions of the MB and delivers them to the NEA region. We calculated the evolution of the NEAs coming from the different source regions by considering the bodies delivered by the resonances and mean dynamical timescales in the NEA population. Results. Our model is in agreement with the major observational constraints associated with the MB, such as the size distributions of the different regions of the MB and the number of large asteroid families. It is also able to reproduce the observed NEAs with H < 16 and agrees with recent estimations for H < 20, but deviates for smaller sizes. We find that most sources make a significant contribution to the NEAs; however the Inner and Middle belts stand out as the most important source of NEAs followed by the Outer belt. The contributions of the Pristine and Cybele regions are minor. The High-Inclination belt is the source of only a fraction of the actual observed NEAs with high inclination, as there are dynamical processes in that region that enable asteroids to increase and decrease their inclinations.
