AGB超星风是理解恒星晚期演化和星系化学演化的关键之一。但是我们对这个复杂动态的物理过程仍然相当缺乏理解，尚无法从第一原理预测AGB星的星风物质损失率。我们在前期单天线观测中首次得到了典型碳星IRC+10216的毫米波频谱光变曲线，发现毫米波谱线光变与超星风产生区域内的物理和化学过程密切相关，并在此基础上发展了一系列ALMA干涉仪1.3毫米波段后续监测观测项目。本课题将利用ALMA监测结果，进行多波段观测比较，以及数值模拟，将首次揭示这个碳星超星风启动区域的动态特征，并可能直接验证超星风的“脉动激波+尘埃形成”机制。

AGB superwind is one of the keys to understanding the late stage evolution of stars and chemical evolution of galaxies. However, our understanding to this complicated and dynamical physical process is still lacking, such that it is still impossible to predict the AGB superwind mass loss rates from first principle even today. In our previous single dish studies, we have successfully obtained for the first time the millimeter molecular emission-line light curves in the archetypal carbon star IRC +10216. The results indicate that the observed variations are closely related to the physical and chemical processes in the surperwind launching region. We thus have developed a series of ALMA 1.3mm monitoring projects to extend the single dish studies. This proposal will combine the ALMA results with multi-wavelength comparison and numerical simulation, to achieve the first comprehensive description of the dynamical characteristics of the superwind launching region, and possibly directly verify the "pulsation shocks + dust formation" model of super-wind launching.