Speaker
Andreas Weiler
(TU Munich, Germany)
Description
Neutron stars and white dwarfs do not just produce axions—they change how axions behave. At high baryon density, the axion potential shifts and nucleon properties are modified, which can alter compact-star structure and amplify axion–nucleon interactions. That means more axion emission in supernovae and stronger, model-independent bounds. I will also outline a simple in-medium axion EFT that exposes a previously missed tree-level production channel, further sharpening supernova constraints, and will connect these ideas to current searches across the stellar graveyard.
