类太阳振动是由恒星表?湍流运动激发的振动形式，在?质量恒星的主序阶段和巨星阶段普遍存在。星震学主要探测恒星的内部结构，为研究恒星对流、元素混合、磁活动、?动 量演化等问题提供了独特的思路。此外，星震学可以确定较准确的恒星参数，确定恒星演化 阶段，?来研究银河系演化等问题。 随着?量空间卫星数据释放，现有的研究类太阳振动恒星的?具遇到了挑战，需要借助?动化程度更?的?段提取观测信息。在本论?中，我们主要开发了提取星震学观测参数的程序，并改进了参数估计的算法，并对 Kepler 卫星的观测数据进?研究。我们?先研究了?个亚巨双星系统 KIC 7107778，其功率谱呈现出了两颗恒星的振动模式，再使?恒星模型分析其振动?为。我们分析了 Kepler 数据中所有的亚巨星，建?了亚巨星振动参数的星表，并研究其混合模式振动的诊断能?。我们还进?步研究了 Kepler 数据?所有的红巨星，提取了径向模式振动的参数，分析了它们与演化阶段的关系。本?的主要结论如下： （1）KIC 7107778 是?个孪?双星系统，包含两颗振动参数与恒星参数极其接近的恒星。两颗恒星的主要参数分别为 M A = 1.42 ± 0.06 M ⊙ ，M B = 1.39 ± 0.03 M ⊙ ，R A = 2.93 ± 0.05 R ⊙ ，R B = 2.76 ± 0.04 R ⊙ ，t A = 3.32 ± 0.54 Gyr 以及 t B = 3.51 ± 0.33 Gyr。其质量相差仅约 ～1%。我们使??分法的原理寻找 KIC 7107778 的最优模型，借助最优模型，多数 l = 1 混合模式均可成功证认。这是观测到的第?颗亚巨星震学双星。 （2）Kepler 观测的 42 颗亚巨星的振动频率可以准确估计，?线宽和振幅的误差相对较?。频率的误差中值为 0.16 μHz，线宽和振幅的相对误差分别为 36% 和 10%。亚巨星的混合模式频率随年龄演化较快，通过在 g 模式频率与 ?ν 的关系图上?较恒星演化轨迹，可以实现快速估计亚巨星的质量。 （3）Kepler 巨星的径向振动模式频率可以准确估计，线宽和振幅的误差相对较?。对于红巨星，频率的误差中值为 0.019 μHz，线宽和振幅的相对误差分别为 27% 和 8%；?对于红团簇??，三者分别为 0.024 μHz、28% 和 9%。根据初步分析，在红巨星与红团簇巨星中，描述恒星振动的特征量 ? 和径向模式平均线宽 ?Γ? 呈现出不同的分布，这?现象不仅与表?特征 T eff 和 log(g) 相关，也与内部物理量有关，其具体原因有待借助恒星模型进?步研究。 通过本?作，我们发展和完善了测定恒星振动参数的?法，并以此为?具，分析了?颗双星、亚巨星和红巨星的振动?为。借助本?作的结果，可以开展后续的星震学诊断?作。

Solar-like oscillation is excited by turbulent convection in the near-surface region and exists in the main sequence and the giant phases of low-mass stars. Asteroseismology is one of the fundamental tools to probe inner structure, providing a unique perspective of convection, element mixing, magnetic activity, angular momentum transport and other problems related to stellar physics. Accurate stellar parameters together with evolutionary stages, determined with asteroseismology, offer critical insight into galactic study. With space-bourn telescopes, the wealth of photometric data require highly automated pipelines to extract seismic information for solar-like oscillators. To this end, we developed an algorithm to extract seismic parameters and improve parameter estimation. In this thesis, we first analysed a binary subgiant system KIC 7107778 and constructed stellar models to interpret its oscillation features. Then we constructed a catalog comprising the oscillation parameters of all Kepler subgiants and further dissected the diagnostic potential of mixed modes. Lastly we analysed the radial oscillation of all Kepler red giants and explored it as a function of evolutionary stage. Our main conclusions are listed as follows. (1) KIC 7107778 comprises almost identical subgiant twins, with extremely close similarity. Stellar parameters for the two subgiant stars are: M A = 1.42 ± 0.06 M ⊙ , M B = 1.39 ± 0.03 M ⊙ , R A = 2.93 ± 0.05 R ⊙ , R B = 2.76 ± 0.04 R ⊙ , t A = 3.32 ± 0.54 Gyr and t B = 3.51 ± 0.33 Gyr. The mass difference of the system is ～1%. Most l = 1 mixed modes were identified with models searched using a bisection method. The system is the first asteroseismic subgiant binary to be detected. (2) For the oscillation parameters of Kepler subgiants, the mode frequencies can be precisely estimated compared to the mode line widths and the mode amplitudes. The uncertainty of mode frequencies has a median value of 0.16 μHz. The relative uncertainties of mode line widths and mode amplitudes are 36% and 10%, respectively. The mixed mode frequency is a sensitive probe for both age and mass. We constructed a g mode frequency - ?ν diagram for all subgiants from which the mass can be estimated effortlessly. (3) For the radial oscillation parameters of Kepler red giants, the mode frequencies can also be precisely estimated. For Hydrogen-shell burning red giants, the uncertainty of the mode frequencies has a median value of 0.019 μHz. The relative uncertainties of the mode line widths and mode amplitudes are 36% and 10%, respectively. For Helium-core burning red clumps, they are 0.024 μHz, 28% and 9%. According to a preliminary analysis, the epsilon ? and the average line width ?Γ? show distinct distributions in the red giant and red clump populations respectively. We attributed the cause to the difference in Teff and log(g) which are sensitive to the surface layers, and the physical quantities describing stellar inside as well. In our future work, we will carefully study this sample with stellar models. In this thesis, we developed the methods to estimate oscillation mode parameters, and implement them in the asteroseismic analyses of KIC 7107778, the subgiants, and the red giants. Future works may include various asteroseismic diagnostics with the derived parameters.