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，即太阳和包括磁变星在内的各种恒星，而矮星和早期类型的恒星，都在以各种本征模式振荡。这开启了被称为“日震学”和“星震学”的新研究领域，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那些恒星的内部，而这些恒星是任何其他观测都无法获得的。我们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论，并用这些地震学方法研究太阳和恒星的内部结构。下面给出我们的结果的简要描述。我们讨论了r模振荡对快速自转早型恒星谱线轮廓的影响，作为对这些恒星光谱中谱线轮廓变化的可能解释。2.提出了一种有效的识别对…有贡献的本征模的方法基于时间和波长的傅里叶分析，线型中的离子更多。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MDO在整个Oph的静止阶段都对线条的丰富变化做出了贡献。4.提出了一种求解太阳p模谱反问题的方法，并利用渐近分析方法推导出太阳内部声速分布。此外，还研究了该方法在实际数值处理中的性质。5.将上述方法应用于已发表的观测数据，并与标准模型的声速分布进行了比较。6.我们发展了另一种逆方法，该方法具有一般可能的目标，但仅限于线性逆问题。7.我们发展了一种求解白矮星g模谱反问题的方法，利用渐近分析来推断这些恒星中Brunt-Vaisala频率的分布。8.对磁性AP星的快速振荡进行了分析，以更新模式识别。较少

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