Collaborative Research: Making a Habitable Planet - The Evolution of the Volatile Inventory in Gas-Rich Planet-Forming Disks

现在很清楚，有大量的行星围绕着与我们太阳相似的恒星运行。该计划旨在了解这些行星是如何诞生的，以及孕育生命所需的关键元素，如碳，氧，氮和氢，是否可能在它们诞生时存在。重点将是通过研究组成这些元素的分子如何被纳入小型岩石体中，从而形成类似地球的行星的早期步骤。该方案将把世界级天文望远镜的联合收割机观测与最先进的详细计算模型结合起来。该计划将促进更好地了解像我们这样的行星是如何诞生的。这项工作的核心部分是培养下一代具有不同背景的科学家，这些科学家代表了研究和教学的未来。这项合作努力融合了布莱克和伯金小组的工作。 这使得使用凯克和阿尔马，可以解释使用详细的理论模型，从不到几个Au的气体排放的观测勘探。 他们将生成数千个物理/时间依赖的化学模型，跨越参数空间，他们将开发/实施微行星形成和冰封存的处方。 从这个网格的丰度和排放预测将阐明的C，H，O和N元素池的关键载体/示踪剂的命运。 这将使得能够确定可观测的，质量独立的，小行星形成的特征。 观测工作将针对不同年龄段的来源进行采样。 这将在两个轨道上完成：（1）使用凯克档案，阿尔马档案，新的凯克光谱天文测量数据，该小组已接受的阿尔马周期1和2计划，加上新的建议，阿尔马周期3。 他们将把这些数据与他们的理论网格进行比较，以表征关键挥发物的整体空间分布及其与行星形成的联系。 已有的数据集适合于研究两个来源的磁盘化学。 (2)第二个是基于这样的证据，即腈可能是热气体的关键有机示踪剂，其条件与年轻星星的预期1 Au相当。 他们将使用阿尔马周期2数据来描述这些有机物在热核中的起源，并提供在附近磁盘系统中寻找这种进化示踪剂的证据。

It is now clear that there is an abundance of planets in orbit around stars similar to our own Sun. This program seeks to understand how these planets are born and whether key elements needed to foster life, such as carbon, oxygen, nitrogen, and hydrogen, are likely to be present at their birth. The focus will be on the early steps in the formation of an Earth-like planet by studying how molecules comprising these elements are incorporated into small, rocky bodies. This program will combine observations from world-class astronomical telescopes with state-of-the-art detailed computational models. This program will foster a greater understanding of how planets like our own are born. A central part of this effort is the training of the next generation of scientists with diverse backgrounds that represent the future of research and teaching.The collaborative effort merges the work of the Blake and Bergin groups. This enables observational explorations of gas emission from less than a few AU using Keck and beyond with ALMA, which can be interpreted using detailed theoretical models. They will generate several thousand physical/time-dependent chemical models spanning parameter space, and they will develop/implement prescriptions for planetesimal formation and ice sequestration. The abundance and emission predictions from this grid will elucidate the fate of key carriers/tracers of the C, H, O, and N elemental pools. This will enable the determination of observable, mass independent, signatures of planetesimal formation. The observational efforts will target sources sampling a range in age. This will be done in two tracks: (1) Using the Keck archive, the ALMA archive, new Keck spectro-astrometric data, the team's accepted ALMA Cycle 1 and 2 programs, plus new proposals for ALMA Cycle 3. They will compare these data to their theoretical grid to characterize the overall spatial distribution of key volatiles and their links to planet formation. Data sets already in hand are suitable to study disk chemistry in two sources. (2) The second is based on evidence that nitriles might be key organic tracers of hot gas that has conditions comparable to those expected 1 AU from a young star. They will use ALMA Cycle 2 data to characterize the origin of these organics in hot cores and provide to search for evidence of this evolutionary tracer in nearby disk systems.