长周期彗星各向异性的形成过程解释
Anisotropy of Long-period Comets Explained by Their Formation Process
摘要：
来自奥尔特云的长周期彗星被认为是在黄道面的行星区形成的微行星。我们已经调查了由于银河潮汐这些机构的轨道演化。推广了Higuchi等人（2007）的理论，推导了远日点方向银河经纬度的解析解，即$L$和$B$。使用的解析解，我们表明，$L$和$B$的演化周期的比率是非常接近的初始偏心率$e_i\simeq 1$，是真实的奥尔特云彗星的2或$\infty$。根据$L$和$B$的关系，我们预测返回行星区的奥尔特云彗星集中在黄道面和第二个平面上，我们称之为“空黄道”。“这包括黄道绕银河系极点旋转180 $^\circ$。我们的数值积分证实，径向分量的银河潮汐，这是被忽略的解析解的推导，是不够强，以打破$L$和$B$解析推导之间的关系。对观测数据的简要检查表明，在黄道和空黄道附近都有集中。我们还表明，异常的分布$B$的长周期彗星的几位作者提到的两个平面上的浓度比以前的解释更一致的解释。
英文摘要：
Long-period comets coming from the Oort cloud are thought to be planetesimals formed in the planetary region on the ecliptic plane. We have investigated the orbital evolution of these bodies due to the Galactic tide. We extended Higuchi et al. (2007) and derived the analytical solutions to the Galactic longitude and latitude of the direction of aphelion, $L$ and $B$. Using the analytical solutions, we show that the ratio of the periods of the evolution of $L$ and $B$ is very close to either 2 or $\infty$ for initial eccentricities $e_i\simeq 1$, as is true for the Oort cloud comets. From the relation between $L$ and $B$, we predict that Oort cloud comets returning to the planetary region are concentrated on the ecliptic plane and a second plane, which we call the "empty ecliptic." This consists in a rotation of the ecliptic around the Galactic pole by 180$^\circ$. Our numerical integrations confirm that the radial component of the Galactic tide, which is neglected in the derivation of the analytical solutions, is not strong enough to break the relation between $L$ and $B$ derived analytically. Brief examination of observational data shows that there are concentrations near both the ecliptic and the empty ecliptic. We also show that the anomalies of the distribution of $B$ of long-period comets mentioned by several authors are explained by the concentrations on the two planes more consistently than by previous explanations.
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