Diagnostics of the Internal Structure of the Sun and Stars using their Oscillations

近年来，非常精确的观测揭示了这样一个事实，即太阳和各种恒星，包括磁变星，而矮星和早期型恒星，都在以各种本征模振荡。这开辟了称为“日震学”和“星震学”的新的研究领域，在这些领域中，我们试图通过分析太阳和恒星的本征振荡来探测太阳和恒星的内部，这是任何其他观测都无法达到的。本项目的目标是从观测和理论上建立日震学和星震学的方法，并通过这些地震学方法研究太阳和恒星的内部结构。我们的结果的简要说明如下。讨论了r模振荡对快速旋转早型星光谱线轮廓的影响，作为这类星光谱线轮廓变化的一种可能解释。2.我们发展了一种有效的方法来识别本征模， 关于我们 离子线配置文件，基于傅立叶分析的时间和波长。3.将上述方法应用于be星的观测数据，成功地识别出了一些本征模。特别是，我们发现，一组相同的mdos有助于线轮廓变化所有通过一个静止阶段的OPH。4.本文提出了一种利用渐近分析方法求解太阳p模谱反问题，从而推断太阳内部声速分布的方法。进一步研究了其它方法在实际数值处理中的性能。5.我们将上述方法应用于已发表的观测数据，并将所得声速分布与标准模型的声速分布进行了比较。6.我们开发了另一种逆方法，它具有一般可能的目标，但仅限于线性逆问题。7.本文发展了一种求解白色矮星g模谱反问题的方法，利用渐近分析，推断出这些恒星的Brunt-Vaisala频率分布。8.分析了磁性Ap星的快速振荡，以更新模式识别。少

In recent years, very accurate observations revealed the fact that the sun and various kind of stars, including magnetic variables, while dwarfs and early-type stars, are oscillating in their various eigenmodes. This opened new fields of research called "helioseismology" and "asteroseismology", in which we try to probe interiors of the sun and those stars, which had been inaccessible to any other observation, by analyzing their eigenoscillations. The objective of our project has been to construct methodology in helioseismology and asteroseismology both observationally and theoretically, and to study internal structures of the sun and stars by those seismological approach. A brief description of our results are given below.1. We discussed effect of r-mode oscillations to line profiles in rapidly rotating early-type stars, as a possible explanation to line profile variation in spectra of those stars. 2. We developed an effective method of identifying eigenmodes which contribute to variat … More ions in line profiles, based on Fourier analysis in time and wavelength. 3. The method described above was applied to observational data of be stars, and we succeeded in identifying some eigenmodes. Particularly, we found that an identical set of mdoes contributes to line profily variation all through a quiescence phase of Oph. 4. We developed a method of solving an inverse problem of solar p-mode spectra, utilizing asymptotic analysis, to infer the sound velocity distribution in the solar interior was developed. Further, the property of othe method in practical numeric process was studied. 5. We applied the method described above to a published observational data, and compared the resultant distribution of sound velocity with that of a standard model. 6. We developed another inverse method which has general possible targets, though restricted to linear inverse problem. 7. We develope a method of solving an inverse problem of g-mode spectra of white dwarfs, utilizing asymptotic analysis, to infer the distribution of Brunt-Vaisala frequency in those stars. 8. Rapid oscillations in magnetic Ap stars are analyzed to renew mode identification. Less