Collaborative Research: The Physics of Accretion Disks

合作研究：吸积盘的物理学

• 批准号: 0908869
• 负责人: John Hawley
• 金额: $ 23.02万
• 依托单位: University of Virginia Main Campus
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 2009
• 资助国家: 美国
• 起止时间: 2009-08-01 至 2016-07-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=0908869&HistoricalAwards=false
• 关键词: Collaborative; Research; Physics; Accretion; Disks

AST-0908336/0908869Krolik/HawleyArmed by an understanding that the fundamental mechanism of accretion is angular momentum transport due to magnetohydrodynamic (MHD) turbulence driven by the magneto-rotational instability, it has become possible to investigate at a detailed level the astrophysical properties of accretion onto black holes. With previous NSF support, this team has developed a suite of Newtonian and general relativistic MHD numerical simulation codes suitable for exploring the global properties of accretion flows onto black holes and the jets they sometimes generate. This collaborative project, led by Dr. Krolik, will now extend prior work to consider accretion thermodynamics and energetics, the impact of large-scale magnetic fields, and how an accretion flow oriented obliquely to the black hole rotation axis at large distances interacts with Lense-Thirring torques. Emphasis will be placed throughout on creating quantitative links between dynamical simulation data and observable properties.This work should provide genuine guidance for the controversy over how much large-scale magnetic flux may be brought deep into the accretion flow. It should also reveal how accretion flows stressed by magnetic fields with intrinsic large-scale structure may differ from those without. In addition, computing MHD stresses within the accretion flow is essential to the question of the extent of disk bending by gravitomagnetic forces, and it should soon be possible to calculate disk structure with sufficient resolution to address this issue.Both simulation codes and data from specific models will be made available to the community, strengthening the software infrastructure of the discipline. The project will provide graduate student training in numerical simulation techniques. Successful public outreach efforts based on simulation results will continue, including planetarium shows and television documentaries.

AST-0908336/0908869KROLIK/HAWLEYARMARMARMARMARMARMARMARMANTIONION驱动的磁性水力动力学（MHD）湍流是由磁性 - 旋转不稳定驱动的，这是有可能的稳定级别的稳定级别的黑色态度的详细级别的质量，这是可能的。 借助以前的NSF支持，该团队开发了一套牛顿和一般相对论的MHD数值模拟代码，适合探索积聚流的全局属性，并有时会生成的黑洞及其喷气式飞机。 由Krolik博士领导的这个合作项目现在将扩展先前的工作，以考虑积聚热力学和能量学，大规模磁场的影响，以及在大距离处倾斜的吸积流向大距离旋转轴的倾斜如何与透明折射的摩尔克斯相互作用。 将重点放在整个动力学模拟数据和可观察到的属性之间建立定量联系。这项工作应为有关多少大规模磁通量的争议提供真正的指导。 它还应揭示磁场固有大规模结构压力的积聚流如何与没有的磁场不同。 此外，吸积流中的计算MHD应力对于引力磁力弯曲程度的问题至关重要，并且应该很快就可以通过足够的解决方案来计算磁盘结构以解决此问题。这些问题的模拟代码和数据都将提供给社区的特定模型，可为社区提供，从而增强了纪律的软件基础结构。 该项目将提供数值模拟技术的研究生培训。 基于模拟结果的成功公开外展工作将继续，包括天文馆表演和电视纪录片。