中文摘要：

利用一种非局部和非定常的恒星对流理论，计算了0．6—3．0M⊙恒星演化模型的线性非绝热脉动．结果表明，赫罗图上脉动不稳定带右方的脉动不稳定的低温恒星可以分成2大类（群）．一类由主序矮星、亚巨星和中低光度红巨星组成的类太阳振荡恒星，它们的中高阶（径向阶nr≥12）P模是脉动不稳定的，而低阶（nr≤5）模是脉动稳定的；另一类是由亮的红巨星和渐近巨星支星（AGB）组成的类长周期变星，它们的低阶模（nr≤5）是脉动不稳定的，而高阶模（nr≥12）却是脉动稳定的．能利用对流与脉动的耦合统一解释造父变星脉动不稳定带红边界、类太阳和类长周期变星脉动．对赫罗图右方的低温恒星的中低阶P模振荡，对流与脉动的耦合是主要的脉动激发和阻尼机制，而湍流的随机激发机制仅对类太阳振荡高阶P模重要．

英文摘要：

The linear stability analysis of the radial and non-radial oscillations for the evolutionary models of the star with a mass of 0.6-3 M⊙ is taken by using a nonlocal and time-dependent convection theory. The results show that the unstable low-temperature stars on the right side of instability strip can be divided into two groups. One is the solar-like oscillation stars composed of the main-sequence dwarfs, subgiants and low- and intermediate-luminous red giants, which are unstable in the intermediate- and high-order （n 〉 12） p-modes and stable in the low-order （n 〈 5） p-modes. Another is the Mira-like stars composed of the lulninous red giants and AGB stars, which are just contrary to the solar-like stars, unstable in the low-order （n 〈 5） p-modes and stable in the intermediate- and high-order （n ≥ 12） p-modes. The red edge of Cepheid （d Seuti） instability strip, the oscillations of solar-like and Mira-like stars can be explained uniformly by the coupling between convection and oscillations （CCO） of instability strip, CCO is the dominant For the low-temperature stars on the right side excitation and damping mechanism for the low- and intermediate-order p-modes, and the turbulent stochastic excitation becomes important only for the high-order p-modes of solar-like oscillations.