Abstract Details
| Name: Sandeep Kumar Kataria Affiliation: JAP-IIA, Bangalore Conference ID: ASI2016_551 Title : Studying the Formation and Structure of Bars in Dark Matter Dominated Spiral Galaxies using Gadget-2 Simulations Authors and Co-Authors : Sandeep Kumar Kataria(JAP-IIA,Bangalore) Mousumi Das(IIA,Bangalore) Lukas Konstandin(University of Exeter) Abstract Type : Poster Abstract Category : Extragalactic astronomy Abstract : We present N body simulations of bar formation in dark matter dominated galaxies which is very less understood with theory. Bars are elongated features found in the centers of spiral galaxies as a result of disk instabilities. Nearly two thirds of all observed spiral galaxies in the nearby universe have bars. The main goals of our study is to investigate the effect of various halo parameters such as halo concentration, triaxiality, mass and profile on the formation of bars in disk galaxies. We will compare our results of bar morphologies and bar lengths in dark matter dominated galaxies to those in found in normal galaxies. The first part of the simulation involves the generation of isolated galaxies using GalIC code (D. Yurin and V. Springel), which contains stellar disc and dark matter particles. The second part consists of evolving these galaxy models with N-body/SPH code(Gadget-2, V. Springel) up to time scale of 10 Gyr. We studied effect of the following halo parameters. (i) Halo Concentration : We first generated the disk galaxies with different halo concentration varying from c= 5 to 20 where c= R_{vir}/ R. We evolved these models up to 10 Gyr. We found that as the halo concentration increases, the bar formation is suppressed. (ii) Halo Triaxiality: In this case also we made different galaxy models with having prolate and oblate shape having axis ratios from 0.8 to 1.2. We are evolving these galaxy models and continuing with analysis. In future we will include a gas component in our simulations in order to study how the gas affects the overall bar morphology and the formation of other disk instabilities. In this presentation we discuss some early results of our study. |