Convection, Oscillations and GONNNNG

对流、振荡和 GONNNNG

• 批准号: 0605738
• 负责人: Robert Stein
• 金额: $ 43万
• 依托单位: Michigan State University
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 2006
• 资助国家: 美国
• 起止时间: 2006-07-01 至 2012-06-30
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=0605738&HistoricalAwards=false
• 关键词: Convection; Oscillations; GONNNNG

The long-term goal of this work is an understanding of the magneto-hydrodynamics ofthe solar surface at scales from granules to sup-granules. Here sophisticated numericalsimulations which include realistic three-dimensional, compressible, magneto-convectionwill be used to model the solar surface and investigate the interaction of convection,magnetic fields, and oscillations. The simulations will be used to interpret observationsfrom GONG, SOHO/MDI, and the Swedish 1m Solar Telescope, to test inversionprocedures, and model the subsurface behavior of solar magneto-convection. Specificobjectives include: 1) To uncover the physical processes that determine the solar surfacestructure through the interaction of convection and magnetic fields on scales fromgranulation to supergranulation. 2) To improve our ability to probe the internal structureof the Sun via helioseismology. 3) To calibrate local helioseismic inversion proceduresfor determining temperatures, flows and magnetic fields near the solar surface. 4) Toinvestigate p-mode physics (dynamic, magnetic and radiative effects on modefrequencies, amplitudes and line asymmetries). 5) To probe the creation, emergence,dispersion and disappearance of magnetic flux in the quiet Sun. And 6) to examine theorigin and maintenance of the magnetic network.The data sets from these simulations will be made available to the community. Thedesign of future solar telescopes will be facilitated through the quantitative informationon observables that will result from this work. These calculations will also improve spaceweather modeling by providing realistic statistical boundary conditions for numericalstudies of the dynamic solar chromosphere and corona.

这项工作的长期目标是在从颗粒到超颗粒的尺度上理解太阳表面的磁流体动力学。在这里，复杂的数值模拟，包括真实的三维，可压缩，磁对流，将被用来模拟太阳表面，并研究对流，磁场和振荡的相互作用。这些模拟将被用来解释GONG、SOHO/MDI和瑞典1M太阳望远镜的观测结果，以测试逆过程，并模拟太阳磁对流的次表层行为。具体目标包括：1)通过对流和磁场在从颗粒化到超颗粒化的尺度上的相互作用，揭示决定太阳表面结构的物理过程。2)通过日震学提高我们探测太阳内部结构的能力。3)校准用于确定太阳表面附近的温度、流动和磁场的局部日震反演程序。4)研究p模物理(动力学、磁效应和辐射效应对模频率、振幅和线不对称性的影响)。5)探索宁静太阳中磁通的产生、出现、弥散和消失。以及6)检查磁力网络的起源和维护。这些模拟的数据集将向社区提供。未来太阳望远镜的设计将通过这项工作将产生的关于可观测对象的定量信息来促进。这些计算还将通过为动态太阳色球和日冕的数值研究提供现实的统计边界条件来改进空间天气模拟。