Bar formation in simulations of interacting galaxies

10th Workshop of the Gravitation and Mathematical Physics Division, Mexican Physical Society

物理学;数学

Luna-Sánchez, Juan Carlos^1,2 ; Rodríguez-Meza, M.A.^1 ; Arrieta, A.^2 ; Gabbasov, R.^3

Departamento de Física, Instituto Nacional de Investigaciones Nucleares, Apdo. Postal 18-1027, México D.F.

11801, Mexico^1

Departamento de Física y Matemáticas, Universidad Iberoamericana, Prolongación Paseo de la Reforma 880, Lomas de Santa-Fe, México, D.F.

C.P. 01210, Mexico^2

Instituto de Ciencias Básicas e Ingenierías, Universidad Autónoma de Pachuca, Ciudad Universitaria, Carr. Pachuca-Tulancingo Km. 4.5 S/N, Pachuca-Hidalgo

C.P. 42184, Mexico^3

关键词: Collision angles;    Collision geometry;    Evolution of galaxies;    Impact-parameter;    Initial conditions;    Major axis lengths;    N-body simulation;    Spherical models;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/545/1/012008/pdf
DOI  :  10.1088/1742-6596/545/1/012008

来源: IOP

【 摘 要 】

In this work we present a study of interacting galaxies using N-body simulations. The initial condition of galaxies are such that they are composed of a bulge, a disc (Freeman model, with no gas), and a halo. For bulge and halo we follow the Dehnen density-pair spherical models. Galaxies are set in a parabolic encounter characterised by the impact parameter and the collision angle subtended by the planes containing each individual galactic discs. The evolution of galaxies are given in terms of the morphology (bar formation, geometry of the bar, minor and major axis length), and the kinematical bar rotation. We show how this characteristics depend on the collision geometry. The dynamics of the collision is given in terms of individual rotation curves, dispersion of velocities of the disc and mass function as functions of the distance to the center of mass of each individual galaxy.