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，原行星盘尘埃分布的子结构是常见的。这些子结构显示出不同的形式，流行度，位置，尺度和振幅，围绕具有不同性质的恒星，如恒星光度和年龄（安德鲁斯2020）。虽然行星-盘相互作用是这些结构起源的流行解释，但有几种理论替代方案，目前真实的起源仍然未知（Pinilla & Youdin 2017），行星只在一个原行星盘中发现（Keppler等人，2018年）。该项目的目的是使用化学模型与流体动力学和尘埃演化模型作为关键的关键，以区分所有这些模型的观察到的子结构的起源。这项研究与新的阿尔马MAPS数据和即将到来的阿尔马AGE-PRO数据是及时的，这些数据旨在绘制化学结构图并在行星形成尺度上限制天然气储层的性质，在各种原行星盘中。用简单的气体和尘埃配方对盘化学进行的参数研究表明，尘埃和气体的耗尽使盘的这些部分对恒星和外部辐射更加透明（紫外线和X射线），因此这些地区变得更温暖。这将直接影响不同丰富挥发物（如水和一氧化碳）的冰线位置，因此也将影响这些盘内形成的行星的组成。相反，在颗粒集中的区域中，盘温度降低并且一些挥发物被隔离在颗粒中（Facchini等人，2018年，Alarcón等人，2020年）。目前的化学模型只详细探讨了行星-盘相互作用的情况，并进行了一些简化。在这篇论文中，我们将探讨不同来源的压力颠簸的影响，包括行星，死区，纬向流，涡。我们的目标是了解这种压力颠簸的性质（当它们形成时，它们的寿命有多长，振幅，位置）如何影响气体和尘埃分布，磁盘温度和原行星盘中几种挥发物的化学丰度。我们把兴趣放在特定的原子和分子线上。例如，碳氧比是为数不多的行星属性之一，可以提供有关行星形成历史的有用信息，并且可以在行星和磁盘中测量（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).