论文标题
矮星谷的动力来源
Dynamical origin of the Dwarf Planet Ceres
论文作者
论文摘要
与主皮带中其他小行星相比，矮星谷谷揭示了氨和其他独特特性的存在，这表明它不是原位形成的。我们对外太阳系的早期动力学演变进行建模，以研究可能的动力学机制，以将静脉区域的小行星带植入ceres大小的行星。我们计算出，在小行星带中捕获的谷物大小的行星群的比例在2.8e-5至1.2e-3的范围内，具体取决于外行星磁盘的初始位置。被捕获的物体具有70％的半轴轴介于2.5至3 au之间的可能性，其偏心率小于0.2的偏心率的可能性为33％，并且具有小于10度的轨道倾斜度的概率为45％。假设在跨性别磁盘的内部存在3,600个CERES大小的行星，与Nesvorny＆vokrouhlicky（2016）一致，跨性别型磁盘的估计，我们的估计捕获概率，我们的估计捕获概率和最终的80％DEPETIENS在Plane cartients ertectients erterientients ertientients cartients Insteritient中的最终迫切性，并导致giant的最终迫切性，该皮带是捕获的。分别位于内部，中部和外带，分别为15％，34％和51％。
The Dwarf Planet Ceres revealed the presence of ammonia and other unique properties compared to other asteroids in the main belt which suggests that it was not formed in situ. We model the early dynamical evolution of the outer Solar System to study possible dynamical mechanisms to implant a Ceres-sized planetesimal in the asteroid belt from the trans-Saturnian region. We calculate that the fraction of the population of Ceres-sized planetesimals that are captured in the asteroid belt is in the range of 2.8e-5 to 1.2e-3 depending on the initial location in the outer planetesimal disk. The captured bodies have a 70% probability to have a semimajor axis between 2.5 and 3 au, a 33% probability to have an eccentricity smaller than 0.2 and a 45% probability to have an orbital inclination smaller than 10 degrees. Assuming the existence of 3,600 Ceres-size planetesimals in the inner part of the trans-Saturnian disk, consistent with the estimate of Nesvorny & Vokrouhlicky (2016) for the trans-Neptunian disk, our estimated capture probability and a final 80% depletion of the asteroid belt during the subsequent giant planet instability, lead to capture 1 Ceres in the asteroid belt, with a probability of 15%, 34%, and 51% to be located in the inner, middle and outer belt respectively.
