2018/11/30 by Kuantay Boshkayev, Daniele Malafarina
Physics and Astronomy · #Accretion (finance) #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Circular motion #Classical mechanics #Cosmology and Gravitation Theories #Dark matter #Dark matter halo #Galactic Center #Galaxy #Galaxy formation and evolution #Galaxy rotation curve #Halo #Milky Way #Physics #Proper motion #Pulsars and Gravitational Waves Research #Schwarzschild radius #Stars #Supermassive black hole #gr-qc
paper · pdf · doi:10.1093/mnras/stz219
9 pages, 9 figures
arxiv created 2018/12/19 · openalex publication_date 2019/01/20 · arxiv updated 2019/05/20 · openalex created_date 2019/06/27 · openalex updated_date 2026/08/05
We consider a toy model for the supermassive compact object at the Galactic centre that does not require the presence of a black hole. We assume a matter distribution of weakly interacting particles with a density profile inferred from dark matter profiles in the outer regions. We show that rotation curves close to the centre of the Milky Way Galaxy can be explained within this model. We also show that the motion of test particles (stars) at distances of the order of 100 au cannot be distinguished from the motion of corresponding particles in the Schwarzschild geometry. However, differences arise at shorter distances, suggesting that it could be possible to observationally test the validity of the model in the near future.