Vecchio A, Carbone V, Lepreti F, Primavera L, Sorriso-Valvo L, Veltri P, Alfonsi G, Straus Th
Dipartimento di Fisica, Università della Calabria, and Istituto Nazionale di Fisica della Materia, Unità di Cosenza, 87030 Rende (CS), Italy.
Phys Rev Lett. 2005 Aug 5;95(6):061102. doi: 10.1103/PhysRevLett.95.061102. Epub 2005 Aug 3.
The spatiotemporal dynamics of the solar photosphere is studied by performing a proper orthogonal decomposition (POD) of line of sight velocity fields computed from high resolution data coming from the MDI/SOHO instrument. Using this technique, we are able to identify and characterize the different dynamical regimes acting in the system. Low-frequency oscillations, with frequencies in the range 20-130 microHz, dominate the most energetic POD modes (excluding solar rotation), and are characterized by spatial patterns with typical scales of about 3 Mm. Patterns with larger typical scales of approximately 10 Mm, are associated to p-modes oscillations at frequencies of about 3000 microHz.
通过对从MDI/SOHO仪器获取的高分辨率数据计算出的视线速度场进行适当正交分解（POD），研究了太阳光球层的时空动力学。使用该技术，我们能够识别和表征系统中不同的动力学状态。频率在20 - 130微赫兹范围内的低频振荡主导了能量最高的POD模式（不包括太阳自转），其特征是具有典型尺度约为3Mm的空间模式。典型尺度约为10Mm的较大模式与频率约为3000微赫兹的p模式振荡相关。
