Thermal Relic Density

  • Martin Bauer
  • Tilman Plehn
Part of the Lecture Notes in Physics book series (LNP, volume 959)


After introducing the observed relic density of photons in Sect.  1.3 and the observed relic density of neutrinos in Sect.  2.1 we will now compute the relic density of a hypothetical massive, weakly interacting dark matter agent. As for the photons and neutrinos we assume dark matter to be created thermally, and the observed relic density to be determined by the freeze-out combined with the following expansion of the Universe. We will focus on masses of at least a few GeV, which guarantees that dark matter will be non-relativistic when it decouples from thermal equilibrium. At this point we do not have specific particles in mind, but in Chap.  4 we will illustrate this scenario with a set of particle physics models.


  1. 1.
    Bellazzini, B., Cliche, M., Tanedo, P.: Effective theory of self-interacting dark matter. Phys. Rev. D 88(8), 083506 (2013). arXiv:1307.1129 [hep-ph]
  2. 2.
    Lisanti, M.: Lectures on Dark Matter Physics (2016). arXiv:1603.03797 [hep-ph]
  3. 3.
    Bernal, N., Heikinheimo, M., Tenkanen, T., Tuominen, K., Vaskonen, V.: The dawn of FIMP dark matter: a review of models and constraints. Int. J. Mod. Phys. A 32(27), 1730023 (2017). arXiv:1706.07442 [hep-ph]CrossRefADSGoogle Scholar

Copyright information

© Springer Nature Switzerland AG 2019

Authors and Affiliations

  • Martin Bauer
    • 1
  • Tilman Plehn
    • 1
  1. 1.Institut für Theoretische PhysikUniversität HeidelbergHeidelbergGermany

Personalised recommendations