On the radial acceleration of disk galaxies
  The physical processes defining the dynamics of disk galaxies are still
poorly understood. Hundreds of articles have appeared in the literature over
the last decades without arriving at an understanding within a consistent
gravitational theory. Dark matter (DM) scenarios or a modification of Newtonian
dynamics (MOND) are employed to model the non-Keplerian rotation curves in most
of the studies, but the nature of DM and its interaction with baryonic matter
remains an open question and MOND formulates a mathematical concept without a
physical process. We have continued our attempts to use the impact theory of
gravitation for a description of the peculiar acceleration and velocity curves
and have considered five more galaxies. Using published data of the galaxies
NGC 3198, NGC 2403, NGC 1090, UGC 3205 and NGC 1705, it has been possible to
find good fits without DM for the observed disk velocities and, as example,
also for the extraplanar matter of NGC 3198.
