The mechanisms shaping the cool cores of galaxy clusters and stabilizing them against catastrophic cooling are not yet understood. High resolution X-ray maps of such cores usually show edges known as cold fronts, AGN bubbles, and sometimes also (quasi) spiral features. I will show that (i) such observations indicate the presence of large scale, bulk spiral flows; (ii) such flows naturally explain the core structure and the subtle features observed; and (iii) these flows can stabilize the core, if the bubbles provide sufficient mechanical feedback.