Collaborative EAGER Proposal: The Dead Zones of Protoplanetary Disks are Not Dead - How Turbulence Transports Angular Momentum and Forms Planetesimals

协作式 EAGER 提案：原行星盘的死区并未死——湍流如何传输角动量并形成星子

• 批准号: 1510703
• 负责人: Philip Marcus
• 金额: $ 26.12万
• 依托单位: University of California-Berkeley
• 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: 2015-03-01 至 2017-02-28
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=1510703&HistoricalAwards=false
• 关键词: Collaborative; EAGER; Proposal; Dead; Zones

This EAGER award funds a collaborative study to study the turbulence of gas and dust in the material that will form planets around stars. The mechanism to be studied could be important in forming the small rocky bodies that are the cores of future planets, and whose process of formation is poorly understood. This study has potential impact in understanding the formation of our own Solar System and of the planets around other stars. The research will create a team consisting of undergraduate and graduate students, and postdoctoral scholars. The collaborative nature of our research will synergistically provide opportunities for students at San Francisco State University, a minority-serving non-PHD institution, to work with students and faculty at University of California at Berkeley. The investigators will also train and mentor a postdoctoral researcher.To accomplish their science goals, the team will compute angular momentum transport in a protoplanetary disk (PPD) dead zone filled with large-amplitude turbulence, compute the rate at which dust and rocks accumulate and agglomerate in a turbulent PPD, and compute mixing in a PPD. In particular, they will determine if the ingredients from which chondrules form become sufficiently mixed that their composition agrees with observations. They will also develop the capability to carry out the above-listed calculation of momentum transport efficiently by extending their current spectral code, which works with anelastic flows, to one that works with fully-compressible flows with Mach numbers less than 3 (as in dead zones). The team will develop the capability to carry out the above-listed calculations of planetesimal and chondrule formation efficiently by replacing their "particle-tracking" code with one that models the rocks and dust as different phases of the fluid flow.

这项急切的奖项为一项合作研究提供了资金，以研究将在恒星周围形成行星的材料中气体和灰尘的湍流。 要研究的机制对于形成是未来行星的岩心的小岩石体可能很重要，并且其形成过程对其的理解很少。 这项研究对了解我们自己的太阳系和其他恒星周围的行星的形成具有潜在的影响。这项研究将创建一个由本科生和研究生以及博士后学者组成的团队。我们研究的协作性质将协同为少数派服务的非PHD机构的旧金山州立大学的学生提供协同机会，以与加州大学伯克利分校的学生和教职员工合作。调查人员还将培训和指导博士后研究人员。为了实现他们的科学目标，该团队将计算质体磁盘（PPD）死区的角动量传输，充满了大振幅湍流，计算灰尘和岩石在湍流中积聚和集聚的速度，并在ppd中堆积，并在ppd中混合在一起。特别是，他们将确定面积形成的成分是否充分混合，以使其成分与观察结果一致。 他们还将通过将其当前的光谱代码（与无弹性流程一起使用）使用，该频谱代码将其当前的频谱代码扩展到与完全可压缩的流量（如MACH数量小于3（如死区）一起使用的能力（如死区）。该团队将通过使用将岩石和灰尘作为流体流的不同阶段进行模拟的“粒子跟踪”代码来有效地进行行星和软骨形成的上述计算的能力。