The physical and dynamical properties of the Kuiper belt as a probe of the processes of planet formation.

柯伊伯带提供了一个了解行星形成过程的宝贵窗口。我们将对柯伊伯带天体（KBO）进行地面和航天器观测，以提供太阳系这一区域行星形成过程的详细图像。** 这些观测活动将利用加拿大-法国夏威夷望远镜、GEMINI望远镜和新地平线号航天器，以及一系列设施的辅助观测。* 具体项目包括：*-我们会进行地面观测，以量度KBO的大小及频率分布。特别是比较分布作为轨道类的函数。外太阳系形成的宇宙成因模型表明，柯伊伯带的各种子类在不同的条件下形成，因此形成过程的标志-尺寸分布应该是不同的。我们将比较100至30公里范围内的大小分布，其中吸积/碰撞过程应占主导地位，而在10至1公里范围内，最初可用于形成的总质量是限制参数。应用新技术探测中等大小（~ 100公里）KBO的恒星掩星，探测KBO将使观测到的KBO光度函数与所需的大小分布之间建立联系。目前，红外观测和传统的掩星观测使最大（+1000公里）的KBO的光度和尺寸之间的联系成为可能，比探测柯伊伯带吸积和碰撞之间相互作用的尺寸大得多。新视野号宇宙飞船将探测到一个100公里大小的KBO，这将大大增加我们对这些天体的了解。对表面惊吓、彗星变化、表面特性等的观测都是地面实况，只能通过航天器访问获得。 我们还将在飞行期间以比地面更高的分辨率获得对其他KBO的观测，探索这些系统中的多重性。

The Kuiper belt provides a valuable window into the processes of planet formation. We will conduct ground and spacecraft observations of Kuiper belt objects (KBOs) to provide a detailed picture of the processes of planet formation in this region of the solar system. ******These observational campaigns will make use the Canada France Hawaii Telescope, the GEMINI telescopes and the New Horizons spacecraft, as well as supporting observations from an array of facilities. ******Specific projects include: ******- We will conduct ground based observations to measure of the size-frequency distribution of KBOs. In particular comparing distributions as a function of orbital class. Cosmogenic models of the formation of the outer solar system indicate that various sub-classes of the Kuiper belt formed under different conditions and thus the size distributions, a signature of the formation process, should be different. We will compare the size distributions in the range between 100 and 30km, where the accretion/collision processes should be dominant and at sizes between 10 and 1km where the total mass originally available for formation is the constraining parameter.******- Application of a novel technique for detection of stellar occultations by mid-sized (~100km) KBOs, detection of which will allow a connection between observed luminosity function of KBOs and the desired size distribution. Currently, infrared observations and traditional occultation observations enable the connection between luminosity and size for the largest (+1000km) KBOs, much larger than sizes where the interplay between accretion and collision in the Kuiper belt is probed.******- New Horizons Spacecraft a ~100km sized KBO which will greatly increase our understanding of these objects. Observations of surface scaring, albedo variations, surface properties, etc. are all ground truths that can only be obtained via a spacecraft visit. We will also obtain, during the flight, observations of other KBOs at higher resolution than can be achieved from the ground, probing for multiplicity in those systems.**