2006/11/01 by A. V. Zasov, O. V. Abramova
Physics and Astronomy · #Accretion (finance) #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Brightness #Disc #Elliptical galaxy #Extinction (optical mineralogy) #Galaxies: Formation, Evolution, Phenomena #Galaxy #Optics #Physics #Spiral galaxy #Star formation #Stellar, planetary, and galactic studies #Surface brightness #astro-ph
paper · pdf · doi:10.1134/s1063772906110023
published as Astron.Rep. 50 (2006) 874-886 · 25 pages, 9 figures
openalex publication_date 2006/11/01 · arxiv created 2006/11/18 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
The four well studied spiral galaxies M33, M81, M100, and M101 are used to analyze the dependences of the star-formation rate (SFR) and star-formation efficiency (SFE = SFR/M gas ) on galactocentric distance R and the photometric and some kinematic parameters of galactic disks. The dependences SFR(R) were estimated based on UV and far-infrared data using published extinction-corrected UV brightness profiles of the galaxies. The local SFE values are most closely related to the surface brightness (density) of the galactic disk at a given R, with this dependence being the same for all four galaxies (except for their central regions). In order to explain the observed disk densities in terms of a simple conservative model (“toy model”) for the evolution of the gas density, the local value of the parameter N in the Schmidt law for the disk (SFR ∼ σ ) must not exceed unity. In this case, the observed dependences σ gas (R) and SFE(R) can be matched assuming that accretion is occuring in the central regions of the disks.