Convection, Oscillations and GONNNNG

这项工作的长期目标是了解太阳表面从颗粒到超颗粒尺度的磁流体动力学。在这里，复杂的数值模拟，其中包括现实的三维，可压缩，磁对流将被用来模拟太阳表面和研究对流，磁场和振荡的相互作用。这些模拟将用于解释GONG、SOHO/MDI和瑞典1米太阳望远镜的观测结果，测试反演程序，并模拟太阳磁对流的地下行为。具体目标包括：1）揭示从颗粒到超颗粒尺度上通过对流和磁场的相互作用决定太阳表面结构的物理过程。2)为了提高我们通过日震学探测太阳内部结构的能力。3)校准确定太阳表面附近温度、流动和磁场的当地日震反演程序。4)研究p模式物理学（对模式频率、振幅和线不对称性的动态、磁性和辐射效应）。5)探测宁静太阳中磁通量的产生、出现、分散和消失。以及6）研究磁网络的起源和维持。这些模拟的数据集将提供给社区。未来太阳望远镜的设计将通过这项工作产生的可观测量的定量信息来促进。这些计算还将通过为动态太阳色球层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建模。

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.