论文标题
OSSO XX：Kuiper皮带颜色的含义
OSSOS XX: The Meaning of Kuiper Belt Colors
论文作者
论文摘要
观察结果表明，100公里级的kuiper带对象（KBOS）可以分为（至少）两个颜色组，以后的红色（R，G-I <1.2）和非常红色（VR，G-I> 1.2），反映出其表面组成的差异。人们认为这意味着KBO在相对较大的径向距离r r。形成。 42 <r <47 au的冷古典物主要是VR，r = 30 au时已知的Neptune Trojans主要是R。但是，动态热的KBO表现出R和VR颜色的混合物，并且与R的颜色没有相关性。在这里，我们执行迁移/不稳定模拟，其中kuiper带从扩展的行星磁盘中填充。我们发现，如果在r <r*和r> r*的r <r*和vr对象形成的r对象（30 <r*<40 au）中，可以最好地理解颜色观察。在30 <r*<40 au处提出的过渡将解释为什么动态热的人群中的VR对象比R对象具有较小的轨道倾斜度，因为Neptune的轨道激发因轨道而弱于30 au。讨论了R-VR颜色双峰的可能原因。
Observations show that 100-km-class Kuiper belt objects (KBOs) can be divided in (at least) two color groups, hereafter red (R, g-i<1.2) and very red (VR, g-i>1.2), reflecting a difference in their surface composition. This is thought to imply that KBOs formed over a relatively wide range of radial distance, r. The cold classicals at 42<r<47 au are predominantly VR and known Neptune Trojans at r=30 au are mostly R. Intriguingly, however, the dynamically hot KBOs show a mix of R and VR colors and no correlation of color with r. Here we perform migration/instability simulations where the Kuiper belt is populated from an extended planetesimal disk. We find that the color observations can be best understood if R objects formed at r<r* and VR objects at r>r*, with 30<r*<40 au. The proposed transition at 30<r*<40 au would explain why the VR objects in the dynamically hot population have smaller orbital inclinations than the R objects, because the orbital excitation from Neptune weakens for orbits starting beyond 30 au. Possible causes of the R-VR color bimodality are discussed.
