Astrochemistry: Hydrodynamics, Cosmic ray induced ice chemistry, and Complex Molecules

天体化学：流体动力学、宇宙射线诱导冰化学和复杂分子

• 批准号: 1514844
• 负责人: Eric Herbst
• 金额: $ 37万
• 依托单位: University of Virginia Main Campus
• 依托单位国家: 美国
• 项目类别: Standard Grant
• 财政年份: 2015
• 资助国家: 美国
• 起止时间: 2015-09-15 至 2019-08-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=1514844&HistoricalAwards=false
• 关键词: Astrochemistry; Hydrodynamics; Cosmic; ray; induced

Astrochemistry is the study of the types of molecules and their chemistry throughout the universe. Molecules in far-away regions are interesting in themselves and as probes of the physical conditions in various regions, especially regions known as dense interstellar clouds. Stars and planets form in these clouds, which are full of molecules, some quite exotic by terrestrial standards. The investigators will study the chemistry that occurs as interstellar clouds collapse and warm up. They will determine which chemical reactions are most important and simulate the changes in the chemical composition of these regions. The final products of the cloud collapse are low-mass stars, like the sun, as well as high-mass stars, which are far brighter than the sun. The synthesis of organic (carbon-containing) molecules is of special interest, since these molecules can become part of nascent planets and are often associated with life. One critical aspect of astrochemistry is the use of chemical simulations to reproduce observational studies of molecular abundances in the gas and on dust particles, and so learn about source lifetimes and physical conditions in the interstellar and circumstellar media. The chemical simulations involve the solution of so-called coupled kinetic differential equations, which yields columns, abundances, or even spectra of many molecules as functions of density, temperature, and degree of heterogeneity. Our primary interest will be to study star formation. Given current and future interferometers, emphasis will be placed on studying the dynamics and heterogeneity of sources undergoing star formation, both the low-mass and high-mass categories. In particular, three-dimensional hydrodynamics will be combined with chemical simulations with the initial goal of understanding the chemistry that occurs during the formation of protoplanetary disks in low-mass sources, and infrared dark clouds, high-mass protostellar objects (HMPOs), and hot cores in high-mass sources. A detailed understanding of the chemistry should yield much information about the details of star formation.

天文学是对整个宇宙中分子类型及其化学类型的研究。 遥远地区的分子本身很有趣，并且作为各个地区的物理条件的探针，尤其是被称为密集的星际云的区域。 这些云中形成的恒星和行星充满了分子，有些按照陆地标准形成了异国情调。 研究人员将研究随着星际云崩溃和热身的化学作用。 他们将确定哪些化学反应最重要，并模拟这些区域的化学成分的变化。云倒塌的最终产物是低质量恒星，例如太阳，以及高质量恒星，远比太阳亮得多。 有机（含碳）分子的合成具有特殊意义，因为这些分子可以成为新生行星的一部分，并且通常与生命有关。 天体化学的一个关键方面是使用化学模拟来再现气体和灰尘颗粒上分子丰度的观察性研究，从而了解星际和情节培养基中的源寿命和身体状况。 化学模拟涉及所谓的耦合动力学微分方程的溶液，该方程得出了许多分子的列，丰度甚至光谱，作为密度，温度和异质性程度的函数。 我们的主要兴趣是研究恒星形成。 鉴于当前和将来的干涉仪，将重点放在研究经历恒星形成的来源的动态和异质性，包括低质量和高质量类别。 特别是，将三维流体动力学与化学模拟结合使用，其最初的目标是了解低质量来源中原绝型磁盘在形成过程中发生的化学性质，以及红云，高质量的原始物体（HMPO）和高质量源中的热核。 对化学的详细理解应产生有关恒星形成细节的大量信息。