To explain the observed population of supermassive black holes at , very massive seed black holes or, alternatively, super-Eddington scenarios are needed to reach final masses of the order of M. A popular explanation for massive seeds has been the direct collapse model, which predicts the formation of a single massive object due to the direct collapse of a massive gas cloud. However, simulations over the last years have shown that such a scenario is very difficult to achieve. Therefore, a realistic model of black hole formation should take fragmentation into account, and consider the interaction between stellar-dynamical and gas-dynamical processes. We present here numerical simulations performed with the AMUSE code, employing an approximate treatment of the gas. Based on these simulations, we show that very massive black holes of M may form depending on the gas supply and the accretion onto the protostars.
Boletin de la Asociacion Argentina de Astronomia La Plata Argentina
- Pub Date:
- August 2019
- black hole physics - stars: Population III - methods: numerical;
- Astrophysics - Astrophysics of Galaxies;
- Astrophysics - High Energy Astrophysical Phenomena
- 3 pages, 1 figure, 1 table. Submitted to BAAA (proceedings for the Binational AAA-SOCHIAS meeting 2018)