2017/12/31 by Rong-Gen Cai, Sichun Sun, Yun-Long Zhang · 9 citations
Physics and Astronomy · #Black Holes and Theoretical Physics #Cold dark matter #Cosmology and Gravitation Theories #Dark Matter and Cosmic Phenomena #Dark energy #Dark fluid #Dark matter #De Sitter space #De Sitter universe #Hot dark matter #Lambda-CDM model #Scalar field dark matter #astro-ph.CO #gr-qc #hep-ph #hep-th
paper · pdf · doi:10.1007/jhep10(2018)009
published in Journal of High Energy Physics 2018(10) (Springer Nature) · 28 pages, 2 figures; Matches published version and we thank the referees for many insightful comments; v3: typos in the Friedmann equations are fixed
openalex created_date 2018/01/05 · openalex publication_date 2018/10/01 · arxiv created 2018/12/26 · arxiv updated 2018/12/27 · openalex updated_date 2026/08/06
A bstract We discuss a scenario that the dark matter in late time universe emerges as part of the holographic stress-energy tensor on the hypersurface in higher dimensional flat spacetime. Firstly we construct a toy model with a de Sitter hypersurface as the holographic screen in the flat bulk. After adding the baryonic matter on the screen, we assume that both of the dark matter and dark energy can be described by the Brown-York stress-energy tensor. From the Hamiltonian constraint equation in the flat bulk, we find an interesting relation between the dark matter and baryonic matter’s energy density parameters, by comparing with the Lambda cold dark matter parameterization. We further compare this holographic embedding of emergent dark matter with traditional braneworld scenario and present an alternative interpretation as the holographic universe. It can be reduced to our toy constraint in the late time universe, with the new parameterization of the Friedmann equation. We also comment on the possible connection with Verlinde’s emergent gravity, where the dark matter is treated as the elastic response of the baryonic matter on the de Sitter spacetime background. We show that from the holographic de Sitter model with elasticity, the Tully-Fisher relation and the dark matter distribution in the galaxy scale can be derived.