Colisiones de galaxias esféricas
We used a self-consistent N-body code to simulate encounters of spherical, non-rotating galaxies. The galaxies were represented by Plummer spheres with isotropic velocity distribution; the mass ratios used for the colliding galaxies were 1:1, 1:2, 1:4 and 1:8. We analyzed the effects on the internal...
Guardado en:
| Autores principales: | , |
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| Formato: | Articulo Comunicacion |
| Lenguaje: | Español |
| Publicado: |
1992
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| Materias: | |
| Acceso en línea: | http://sedici.unlp.edu.ar/handle/10915/143899 |
| Aporte de: |
| Sumario: | We used a self-consistent N-body code to simulate encounters of spherical, non-rotating galaxies. The galaxies were represented by Plummer spheres with isotropic velocity distribution; the mass ratios used for the colliding galaxies were 1:1, 1:2, 1:4 and 1:8. We analyzed the effects on the internal structure of the galaxies caused by collisions that did not result in mergers after a Hubble time (1.5 x 10¹⁰ y). We estimated changes in mass, energy and size, and discussed possible correlations between these properties and the orbital parameters. |
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