N-body modeling of disk and dwarf galaxy minor merger. Chemical radial gradient.

Details N-body modeling of disk and dwarf galaxy minor merger. Chemical radial gradient. N-body modeling of disk and dwarf galaxy minor merger. Chemical radial gradient.

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006yosc.conf...84s&link_type=abstract

13th Young Scientists' Conference on Astronomy and Space Physics, held in Kyiv, Ukraine, April 25-29, 2006, Eds.: Golovin, A.; I

Physics

Space Physics

Scientific paper

We investigated the changes of chemical radial gradient in the disk of a massive galaxy owing to its interaction (merger) with a low-mass satellite with low heavy elements abundances. To consider this problem, a special computer program for dynamical simulation of galaxy merger through the N-body method was developed. This N-body algorithm re- alization also includes the processes of viscosity particle collisions. The disk galaxy and its dwarf satellite are described at the initial time mo- ment as balanced configurations of the Plummer-Kuzmin and Plummer particle distributions, respectively. We also included the conception of heavy elements abundances in particles of N-body dynamical model. We determine the radial gradient of heavy elements abundances in galactic disk after the collision over the set of dynamical particles mixture from both disk and bulge particles and dwarf satellite particles. In the process of disk and dwarf galaxies encounter in our model we observe a distinct lowering of chemical heavy elements abundances in the disk of a massive galaxy at the place of dwarf galaxy position. We compared our results with the observational data for the disk galaxy NGC 2903. In this galaxy the compact area with lowered heavy elements abundances is clearly defined. Thus, we can conclude that the dwarf galaxy absorption at this object has happened less than few billion years ago.

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