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Formación rápida de binarios de agujeros negros supermasivos en fusiones de galaxias con gas
L Mayer1, S Kazantzidis, P Madau
1Institute for Theoretical Physics, University of Zurich, Winterthurestrasse 190, CH-8057 Zürich, Switzerland. lucio@phys.ethz.ch
Science (New York, N.Y.)
|June 9, 2007
Resumen
Los agujeros negros supermasivos (SMBH) forman binarios excéntricos dentro de un millón de años después de las fusiones de galaxias. La dinámica de los gases, no las estrellas, impulsa esta rápida formación binaria en los discos galácticos turbulentos.
Área de la Ciencia:
- La astrofísica es la astrofísica.
- La astrofísica computacional es una astrofísica computacional.
- Evolución de la galaxia Evolución de la galaxia.
Sus antecedentes:
- Los agujeros negros supermasivos (SMBH) residen en la mayoría de los núcleos galácticos.
- Se espera que las fusiones de galaxias formen binarios SMBH que eventualmente se fusionan.
- El mecanismo de unión de los binarios SMBH durante las fusiones de galaxias ricas en gas sigue sin estar claro debido a las complejidades de escala.
Objetivo del estudio:
- Para simular y dilucidar el proceso de formación binaria SMBH durante las fusiones de galaxias ricas en gas.
- Para investigar el papel de la dinámica de los gases frente a la dinámica estelar en la unión binaria SMBH.
- Para modelar la evolución binaria de SMBH hasta escalas de sub-parsec.
Principales métodos:
- Simulaciones hidrodinámicas de galaxias espirales en colisión.
- Seguimiento de la formación y evolución de un binario SMBH.
- Modelado de gas y dinámica estelar a través de una amplia gama de escalas espaciales.
Principales resultados:
- Un disco gaseoso nuclear masivo y turbulento forma una fusión post-galáctica.
- La formación binaria del agujero negro supermasivo (SMBH) ocurre en menos de 1 millón de años.
- El arrastre gravitacional del gas, no de las estrellas, es el principal impulsor de la unión binaria SMBH.
Conclusiones:
- La dinámica de los gases es crucial para la rápida formación de binarios SMBH excéntricos en los centros galácticos.
- Las simulaciones han modelado con éxito la evolución binaria de SMBH hasta escalas de unos pocos años luz.
- Este trabajo aclara un mecanismo clave en las etapas finales de la evolución de la galaxia y SMBH.
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