SPH Simulations of Spherical Bondi Accretion: First Step of Implementing AGN Feedback in Galaxy Formation

Details SPH Simulations of Spherical Bondi Accretion: First Step of Implementing AGN Feedback in Galaxy Formation SPH Simulations of Spherical Bondi Accretion: First Step of Implementing AGN Feedback in Galaxy Formation

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21714248b&link_type=abstract

American Astronomical Society, AAS Meeting #217, #142.48; Bulletin of the American Astronomical Society, Vol. 43, 2011

Statistics

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Our motivation is to numerically test the assumption of Black Hole (BH) accretion (that the central massive BH of a galaxy accretes mass at the Bondi-Hoyle accretion rate, with ad-hoc choice of parameters), made in many previous galaxy formation studies including AGN feedback.
We perform simulations of a spherical distribution of gas, within the radius range 0.1 - 200 pc, accreting onto a central supermassive black hole (the Bondi problem), using the 3D Smoothed Particle Hydrodynamics code Gadget.
In our simulations we study the radial distribution of various gas properties (density, velocity, temperature, Mach number).
We compute the central mass inflow rate at the inner boundary (0.1 pc), and investigate how different gas properties (initial density and velocity profiles) and computational parameters (simulation outer boundary, particle number) affect the central inflow.
Radiative processes (namely heating by a central X-ray corona and gas cooling) have been included in our simulations.
We study the thermal history of accreting gas, and identify the contribution of radiative and adiabatic terms in shaping the gas properties.
We find that the current implementation of artificial viscosity in the Gadget code causes unwanted extra heating near the inner radius.

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