Collisions of non-rotating spherical galaxies
We have used self-consistent numerical simulations of N-body systems to investigate encounters between spherical non-rotating galaxies. In our simulations, the galaxies were represented by Plummer spheres (ρ∝r–5 with isotropic velocity distribution, and we considered collisions along hyperbolic, as...
Guardado en:
| Autores principales: | , |
|---|---|
| Formato: | Articulo |
| Lenguaje: | Inglés |
| Publicado: |
1995
|
| Materias: | |
| Acceso en línea: | http://sedici.unlp.edu.ar/handle/10915/139417 |
| Aporte de: |
| id |
I19-R120-10915-139417 |
|---|---|
| record_format |
dspace |
| institution |
Universidad Nacional de La Plata |
| institution_str |
I-19 |
| repository_str |
R-120 |
| collection |
SEDICI (UNLP) |
| language |
Inglés |
| topic |
Astronomía methods: numerical galaxies: evolution galaxies: interactions galaxies: structure |
| spellingShingle |
Astronomía methods: numerical galaxies: evolution galaxies: interactions galaxies: structure Vergne, María Marcela Muzzio, Juan Carlos Collisions of non-rotating spherical galaxies |
| topic_facet |
Astronomía methods: numerical galaxies: evolution galaxies: interactions galaxies: structure |
| description |
We have used self-consistent numerical simulations of N-body systems to investigate encounters between spherical non-rotating galaxies. In our simulations, the galaxies were represented by Plummer spheres (ρ∝r–5 with isotropic velocity distribution, and we considered collisions along hyperbolic, as well as a few parabolic, orbits. Pairs of galaxies with several different mass ratios (1:1, 1:2, 1:4 and 1:8) were included. We analysed the effects on the internal structure of the galaxies caused by collisions that did not result in mergers after one Hubble time, quantitatively estimating the changes in linear size, mass and energy, and discussing their possible correlations with the orbital parameters. Besides this, we used the results of collisions that ended up in mergers to investigate the structure of the remnants (with respect to binding energy, mass loss, linear size and flattening). We also obtained the density profiles of the remnants, which are well described by an r–γ law profile with 3<γ<3.7. Finally, from the analysis of collisions that ended up in mergers and of those that did not, we established a range of initial velocities and impact parameters that serves as a merging criterion. |
| format |
Articulo Articulo |
| author |
Vergne, María Marcela Muzzio, Juan Carlos |
| author_facet |
Vergne, María Marcela Muzzio, Juan Carlos |
| author_sort |
Vergne, María Marcela |
| title |
Collisions of non-rotating spherical galaxies |
| title_short |
Collisions of non-rotating spherical galaxies |
| title_full |
Collisions of non-rotating spherical galaxies |
| title_fullStr |
Collisions of non-rotating spherical galaxies |
| title_full_unstemmed |
Collisions of non-rotating spherical galaxies |
| title_sort |
collisions of non-rotating spherical galaxies |
| publishDate |
1995 |
| url |
http://sedici.unlp.edu.ar/handle/10915/139417 |
| work_keys_str_mv |
AT vergnemariamarcela collisionsofnonrotatingsphericalgalaxies AT muzziojuancarlos collisionsofnonrotatingsphericalgalaxies |
| bdutipo_str |
Repositorios |
| _version_ |
1764820457697050625 |