2012/09/13 by Sergey Khoperskov, S. A. Khoperskov, А. В. Хоперсков +10 · 27 citations
Physics and Astronomy · #Astrophysics #Astrophysics and Star Formation Studies #Galaxies: Formation, Evolution, Phenomena #Galaxy #Geometry #Physics #Rotation (mathematics) #Spiral (railway) #Spiral galaxy #Stellar, planetary, and galactic studies #Structure formation #Velocity dispersion #astro-ph.CO #astro-ph.GA
paper · pdf · open access · doi:10.1111/j.1365-2966.2012.22031.x
published in Monthly Notices of the Royal Astronomical Society 427(3), 1983-1993 (Oxford University Press) · 14 pages, 21 figures, accepted for publication in MNRAS
arxiv created 2012/09/13 · openalex publication_date 2012/11/20 · arxiv updated 2015/06/11 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Using observational data, we build numerical N-body, hydrodynamical and combined equilibrium models for the spiral galaxy NGC 5247. The models turn out to be unstable as regards spiral structure formation. We simulate scenarios of spiral structure formation for different sets of equilibrium rotation curves, radial velocity-dispersion profiles and disc thicknesses and demonstrate that in all cases the simulated spiral pattern agrees qualitatively with the observed morphology of NGC 5247. We also demonstrate that an admixture of a gaseous component with a mass of about a few per cent of the total mass of the disc increases the lifetime of a spiral pattern by approximately 30 per cent. The simulated spiral pattern in this case lasts for about 3 Gyr from the beginning of the growth of perturbations.