Effect of Particle Traps on the Disk Chemistry and the Future Composition of Planets

最近对原行星盘的观测表明，原行星盘尘埃分布中的亚结构是常见的。这些亚结构在具有不同性质的恒星周围显示出不同的形式、普遍程度、位置、尺度和幅度，例如恒星的光度和年龄(Andrews 2020)。尽管行星-圆盘相互作用是对这些结构起源的一种流行解释，但有几种理论上的替代方案，目前真正的起源仍然未知(Pinilla&Youdin 2017)，而且只在一个原行星圆盘中发现了行星(Keppler等人，2018年)。该项目的目的是使用化学模型以及流体力学和尘埃演化模型作为关键，以区分所有这些模型，以确定所观测到的亚结构的起源。这项研究适时地发布了新的ALMA地图数据和即将到来的ALMA AGE-PRO数据，旨在绘制各种原行星盘中形成行星尺度上的气藏的化学结构并限制其性质。通过简单的气体和尘埃处方对盘化学进行的参数研究表明，尘埃和气体的枯竭使盘的这些部分对恒星和外部辐射(紫外线和X射线)更加透明，因此这些区域变得更温暖。这将对水和一氧化碳等不同丰富挥发物的冰线位置产生直接影响，因此也将影响在这些圆盘内形成的行星的组成。相反，在颗粒集中的区域，圆盘温度降低，一些挥发物被隔离在颗粒中(Facchini等人，2018，Alarcón等人，2020)。目前的化学模型只详细探讨了行星-圆盘相互作用的情况，并进行了几次简化。在这篇论文中，我们将探讨不同起源的压力凸起在圆盘中的影响，包括行星、死区、纬向流和旋涡。我们的目标是了解这种压力碰撞的性质(它们何时形成，它们的寿命，幅度，位置)如何影响气体和尘埃的分布，圆盘温度和原行星圆盘中几种挥发物的化学丰度。我们对特定的原子和分子谱线感兴趣。例如，碳氧比是能够提供关于行星形成历史的有用信息的为数不多的行星属性之一，它可以在行星和盘中进行测量(例如，MadHusudhan等人，2012年，Bergin等人，2016年)。

Recent observations of protoplanetary disks reveal that substructures in the dust distribution of protoplanetary disks are common. These substructures show different forms, prevalence, locations, scales, and amplitudes around stars with different properties, such stellar luminosity and age (Andrews 2020). Although planet-disk interaction is a popular explanation for the origin of these structures, there are several theoretical alternatives and currently the real origin remains unknown (Pinilla & Youdin 2017), and planets have been only found in one protoplanetary disk (Keppler et al., 2018). The purpose of this project is to use chemical models together with hydrodynamical and dust evolution models as crucial keys to differentiate between all these models for the origin of the observed substructures. This research is timely with the new ALMA MAPS data and the incoming ALMA AGE-PRO data, which aim to map the chemical structures and constrain the properties of the gas reservoirs on planet-forming scales, in a variety of protoplanetary disks.Parametric studies of disk chemistry with simple prescriptions of gas and dust have shown that depletions of dust and gas make those parts of the disk more transparent to stellar and external radiation (UV and X-rays), and therefore these regions become warmer. This will have a direct influence on the locations of the ice lines of different abundant volatiles, such as water and carbon-monoxide, and as a consequence it will also affect the composition of the planets forming within these disks. Contrary, in the regions where particles concentrate, the disk temperature decrease and some volatiles are sequestered in the grains (Facchini et al., 2018, Alarcón et al., 2020). Current chemical models have only explored in detail the case of planet-disk interaction, with several simplifications. In this thesis, we will explore the effect of different origins of pressure bumps in the disk, including planets, dead zones, zonal flows, and vortices. We aim to understand how the nature of such pressure bumps (when they form, how long they live, amplitude, location) affects the gas and dust distribution, the disk temperature and the chemical abundances of several volatiles in protoplanetary disks. We place interest on particular atomic and molecular lines. For instance, the carbon-to-oxygen ratio is one of the few planetary properties which can provide useful information on the formation history of a planet, and it can be measure both in planets and disks (e.g., Madhusudhan et al., 2012, Bergin et al., 2016).