PIRSA:16060012

Video URL

https://pirsa.org/16060012

Quantum Field Theory of Interacting Dark Matter/Dark Energy: Dark Monodromies

Kaloper, N. (2016). Quantum Field Theory of Interacting Dark Matter/Dark Energy: Dark Monodromies. Perimeter Institute for Theoretical Physics. https://pirsa.org/16060012

Kaloper, Nemanja. Quantum Field Theory of Interacting Dark Matter/Dark Energy: Dark Monodromies. Perimeter Institute for Theoretical Physics, Jun. 02, 2016, https://pirsa.org/16060012 

          @misc{ scivideos_PIRSA:16060012,
            doi = {10.48660/16060012},
            url = {https://pirsa.org/16060012},
            author = {Kaloper, Nemanja},
            keywords = {Particle Physics},
            language = {en},
            title = {Quantum Field Theory of Interacting Dark Matter/Dark Energy: Dark Monodromies},
            publisher = {Perimeter Institute for Theoretical Physics},
            year = {2016},
            month = {jun},
            note = {PIRSA:16060012 see, \url{https://scivideos.org/index.php/pirsa/16060012}}
          }

Nemanja Kaloper University of California System

Talk numberPIRSA:16060012
DOI10.48660/16060012
Source RepositoryPIRSA
Collection
Talk Type Scientific Series
Subject

Abstract

We discuss how to formulate a quantum field theory of dark energy interacting with dark matter. We show that the proposals based on the assumption that dark matter is made up of heavy particles with masses which are very sensitive to the value of dark energy are strongly constrained. Quintessence-generated long range forces and radiative stability of the quintessence potential require that such dark matter and dark energy are completely decoupled. However, if dark energy and a fraction of dark matter are very light axions, they can have significant mixings which are radiatively stable and perfectly consistent with quantum field theory. Such models can naturally occur in multi-axion realizations of monodromies. The mixings yield interesting signatures which are observable and are within current cosmological limits but could be constrained further by future observations.