标题： 太阳对流的湍流动能谱来自NST观测和现实MHD模拟 显示英文标题

标题： Turbulent Kinetic Energy Spectra of Solar Convection from NST Observations and Realistic MHD Simulations

摘要： 日冕安静状态的湍流特性代表了表面条件的基本状态，也是太阳活动各种过程的背景。 因此，理解这一“基本”状态的特性和动力学对于研究更复杂的现象、光球层和大气中观测现象的形成和发展非常重要。 为了表征湍流特性，我们将从红外TiO观测得到的粒状和次粒状尺度的动能谱与新太阳望远镜（比尔太阳能观测站）和3D辐射MHD数值模拟（'SolarBox'代码）的结果进行比较。 我们发现，数值模拟需要高空间分辨率，网格步长为10 - 25公里，才能再现惯性（科莫戈罗夫）湍流范围。 观测数据需要一个平均过程来去除噪声和潜在的仪器伪影。 结果表明，模拟和观测之间的动能谱有很好的一致性，这为对太阳上更复杂的湍流现象以及可能在其他恒星上的详细联合分析开辟了新的前景。 此外，利用模拟和观测，我们研究了背景磁场的影响，该磁场集中在粒间槽中的自组织复杂结构中，并发现由于磁场的影响，小尺度湍流能量增加，而在较大尺度上减少。 显示英文摘要

摘要： Turbulent properties of the quiet Sun represent the basic state of surface conditions, and a background for various processes of solar activity. Therefore understanding of properties and dynamics of this `basic' state is important for investigation of more complex phenomena, formation and development of observed phenomena in the photosphere and atmosphere. For characterization of the turbulent properties we compare kinetic energy spectra on granular and sub-granular scales obtained from infrared TiO observations with the New Solar Telescope (Big Bear Solar Observatory) and from 3D radiative MHD numerical simulations ('SolarBox' code). We find that the numerical simulations require a high spatial resolution with 10 - 25 km grid-step in order to reproduce the inertial (Kolmogorov) turbulence range. The observational data require an averaging procedure to remove noise and potential instrumental artifacts. The resulting kinetic energy spectra show a good agreement between the simulations and observations, opening new perspectives for detailed joint analysis of more complex turbulent phenomena on the Sun, and possibly on other stars. In addition, using the simulations and observations we investigate effects of background magnetic field, which is concentrated in self-organized complicated structures in intergranular lanes, and find an increase of the small-scale turbulence energy and its decrease at larger scales due to magnetic field effects.