太阳自转对来自GONG、GOLF和MDI观测的日震资料的敏感性分析
Sensitivity analysis of the solar rotation to helioseismic data from GONG, GOLF and MDI observations
摘要：
从日震观测中准确确定太阳辐射区的旋转速率需要高质量的旋转频率分裂以及可靠的反演技术。我们在这里提出的推论的基础上计算的模式参数从2088天长的MDI，宫和高尔夫球的时间序列，拟合估计非常低的频率旋转分裂（nu < 1.7兆赫）。这些低频模式提供了异常质量的数据，因为模式峰的宽度比旋转分裂小得多，因此更容易将旋转分裂与由模式的有限寿命和随机激励引起的效应分开。我们还实施了一种新的反演方法，使我们能够推断出旋转速率的辐射内部的模式集，跨度l=1至25。我们的结果与太阳在大部分辐射区像刚性固体一样旋转并在核心减速（R_sun < 0.2）是一致的。对太阳自转反问题进行了反演的分辨率分析。这种分析有效地建立了反演中包含的模式集与所得推断的灵敏度和信息内容之间的直接关系。我们表明，这样的方法使我们能够确定添加低频和低度p-模式，高频和低度p-模式，以及一些g-模式的太阳辐射区，特别是太阳能核心的导出的旋转速率的影响。我们的结论是，所需的不确定性水平，以推断动力学条件的核心时，只有p-模式被包括在内是不可能在不久的将来达到，因此需要持续的努力对g-模式的检测和表征。
英文摘要：
Accurate determination of the rotation rate in the radiative zone of the sun from helioseismic observations requires rotational frequency splittings of exceptional quality as well as reliable inversion techniques. We present here inferences based on mode parameters calculated from 2088-days long MDI, GONG and GOLF time series that were fitted to estimate very low frequency rotational splittings (nu < 1.7 mHz). These low frequency modes provide data of exceptional quality, since the width of the mode peaks is much smaller than the rotational splitting and hence it is much easier to separate the rotational splittings from the effects caused by the finite lifetime and the stochastic excitation of the modes. We also have implemented a new inversion methodology that allows us to infer the rotation rate of the radiative interior from mode sets that span l=1 to 25. Our results are compatible with the sun rotating like a rigid solid in most of the radiative zone and slowing down in the core (R_sun < 0.2). A resolution analysis of the inversion was carried out for the solar rotation inverse problem. This analysis effectively establishes a direct relationship between the mode set included in the inversion and the sensitivity and information content of the resulting inferences. We show that such an approach allows us to determine the effect of adding low frequency and low degree p-modes, high frequency and low degree p-modes, as well as some g-modes on the derived rotation rate in the solar radiative zone, and in particular the solar core. We conclude that the level of uncertainties that is needed to infer the dynamical conditions in the core when only p-modes are included is unlikely to be reached in the near future, and hence sustained efforts are needed towards the detection and characterization of g-modes.
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