The Evolution of Intermediate Mass Stars

<p>Intermediate mass stars (M ~ 2.0 - 3.0 Msun) provide interesting constraints on stellar rotation and evolution because they live in an important transitional regime. Like massive stars, they rotate rapidly on the main sequence and have convective cores. However, they evolve to become secondary clump stars, where their structure and internal rotation can be measured with the tools of red giant asteroseismology developed for lower mass stars. We have used these tools to track these stars as they evolve, and measured their rotation, activity, and chemical mixing in various phases. I will demonstrate that the slow&nbsp;rotation rates of these stars provide conclusive evidence for some combination of strong post-main-sequence angular momentum loss and differential rotation with depth in convective envelopes, and discuss their core-envelope coupling as a function of time. Finally, I will discuss the relationships between rotation, activity, and mixing in these stars, and their implications for the broader population of massive stars.</p>