%0 Generic
%A Bertschik, Michael
%D 2004
%F heidok:4753
%K Galaxienkollisionen , Galaxienverschmelzungen , MilchstraßensatellitenMinor Merger , structure formation , cosmology , numerical simulation , Milky Way , Milky Way satellites , dark matter
%R 10.11588/heidok.00004753
%T The Kinematical Parameters of Minor Mergers and their Observational Traces
%U https://archiv.ub.uni-heidelberg.de/volltextserver/4753/
%X Parameters of Minor Mergers and their Observational Traces This work was motivated by observations that galaxies like our Milky Way are undergoing merger with galactic satellites and leaving behind observational traces. The thick disk of our Milky Way may be due to a collision with a satellite of substantial mass of the galaxy, i.e. 1:20 to 1:5, what we call a ``minor merger''. First, we derived in cosmological simulations the kinematical properties of dark matter halos that are minor merging and their abundance in space and time. We found that minor merger were most likely at a time 7Gyrs ago and happened typically once for a Milky Way sized halo. Their pericenter distances and their eccentricities varied with time, we found smaller pericenter distances and  more parabolic orbits in the past. The merging rate differed significantly from the simulated and observed merging rate of major merger while the merging parameter roughly matched expectations from major merger. There was no dependency of the angles between orbit and spin axes of the objects found and no dependency of the mass ratios on redshift. We put these informations into more detailed simulations of a stellar galactic disk that merges with a satellite to see whether an observer in the disk is able to observe traces from this minor merger. We found that the satellite particles are hard to distinguish from halo objects, while the LOSVD shows only few traces of satellite remnants. Effects like heating of the galactic disk were clearly visible.