2012/01/31 by Kohei Kamada, Masahide Yamaguchi · 1 citation
Physics and Astronomy · #Astrophysics #Asymmetry #Baryogenesis #Baryon #Baryon asymmetry #CP violation #Cosmology #Cosmology and Gravitation Theories #Dark Matter and Cosmic Phenomena #Dark energy #Dark fluid #Dark matter #Lepton #Mixed dark matter #Particle physics #Particle physics theoretical and experimental studies #Physics #Physics beyond the Standard Model #Quantum mechanics #Scalar field dark matter #Universe #Warm dark matter #astro-ph.CO #hep-ph
paper · pdf · doi:10.1103/physrevd.85.103530
29 pages; v2, references added; v3, published version
openalex publication_date 2012/05/30 · arxiv created 2012/06/26 · arxiv updated 2013/05/29 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
The observational relation between the density of baryon and dark matter in the Universe, \ensuremathΩDM/\ensuremathΩB\ensuremath≃5, is one of the most difficult problems to solve in modern cosmology. We discuss a scenario that explains this relation by combining the asymmetric dark matter scenario and the spontaneous baryogenesis associated with the flat direction in the supersymmetric standard model. A part of baryon asymmetry is transferred to charge asymmetry D that dark matter carries, if a symmetry violating interaction that works at high temperature breaks not only B\mathrm\text\ensuremath-L but also D symmetries simultaneously. In this case, the present number density of baryon and dark matter can be same order if the symmetric part of dark matter annihilates sufficiently. Moreover, the baryon number density can be enhanced as compared to that of dark matter if another B\mathrm\text\ensuremath-L violating interaction is still in thermal equilibrium after the spontaneous genesis of dark matter, which accommodates a TeV scale asymmetric dark matter model.