F. Cruz and H. Velázquez
Instituto de Astronomía, UNAM, Apdo. Postal 877, 22800 Ensenada, B. C., México (fidel@astrosen.unam.mx; hmv@astrosen.unam.mx).
Received, 2004 August 18
Accepted 2004 October 18.
]]> RESUMEN
Hemos abordado la formación de perfiles agudos a través de simulaciones de N-cuerpos, en dos escenarios complementarios: (1) un colapso gravitacional frío alrededor de un agujero negro supermasivo preexistente, y (2) un crecimiento adiabático de un agujero negro en un sistema estelar relajado obtenido de un colapso gravitacional frío. Ambos modelos dan lugar a un perfil de densidad, ργ, con un índice de ley de potencias similar, γ; sin embargo, presentan diferencias cinemáticas y morfológicas.
ABSTRACT
We address the formation of cuspy density profiles, through N-body simulations, in two complementary scenarios: (1) a cold gravitational collapse around a preexisting supermassive black hole, and (2) an adiabatic growth of a central black hole in a relaxed stellar system obtained from a cold gravitational collapse. Both models lead to a density profile, ργ, with a similar power-law index, γ; however, they show kinematical and morphological differences.
Key Words: Galaxies: Elliptical and lenticular, CD — Galaxies: Formation — Galaxies: Nuclei — Methods: Numerical.
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ACKNOWLEDGMENTS
]]> This research was supported by grants DGAPA grant IN113403, UNAM, México.
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