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: 1510708
• 负责人: Joseph Barranco
• 金额: $ 3.83万
• 依托单位: San Francisco State University
• 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=1510708&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.

该 EAGER 奖项资助一项合作研究，研究将在恒星周围形成行星的材料中气体和尘埃的湍流。 待研究的机制对于形成未来行星核心的小型岩石天体可能很重要，但人们对其形成过程知之甚少。 这项研究对于了解我们自己的太阳系和其他恒星周围行星的形成具有潜在影响。该研究将创建一个由本科生、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为旧金山州立大学（一所少数族裔服务的非博士机构）的学生提供与加州大学伯克利分校的学生和教师合作的机会。研究人员还将培训和指导一名博士后研究员。为了实现他们的科学目标，该团队将计算充满大幅湍流的原行星盘（PPD）死区中的角动量传输，计算灰尘和岩石在湍流 PPD 中积累和凝聚的速率，并计算 PPD 中的混合。特别是，他们将确定形成球粒的成分是否充分混合，使其成分与观察结果相符。 他们还将通过将当前适用于滞弹性流的谱代码扩展到适用于马赫数小于 3（如死区）的完全可压缩流的谱代码，开发有效执行上述动量传递计算的能力。该团队将通过将其“粒子跟踪”代码替换为将岩石和尘埃建模为流体流动的不同阶段的代码，开发有效执行上述星子和球粒形成计算的能力。