Astronomy and Astrophysics – Astrophysics
Scientific paper
2004-09-29
Astrophys.J. 615 (2004) L93-L96
Astronomy and Astrophysics
Astrophysics
4 pages, 4 figures, Accepted for publication in ApJL
Scientific paper
10.1086/426119
Using high-resolution N-body/SPH simulations with $2\times 10^6$ particles, we investigate the evolution of stellar and gaseous galactic cores during the hierarchical formation of a spiral galaxy. We find that the galactic core ($r < 300 $ pc) coevolves with the host galaxy. The average mass ratio between the baryonic core and the halo is nearly constant, $\sim $ 0.04 from $z \sim 10$ to $z \sim 2$. However, there are several `rapid-growing phases' during the evolution, in which the rate of mass accretion to the central sub-kpc region is ten times higher ($\sim 1 M_\odot$ yr pc$^{-1}$) than the average accretion rate. The rapid growth of the inner core is associated with the major merger events with a time-delay. We also find that the spin-axis of the gas core frequently changes. As a result, the angular momentum vector of the central part of the galaxy is independent of the rotation of the outer part. Our results suggest that if a constant fraction of the baryonic mass in the central several 100 pc of a galaxy is converted into a massive black hole, the black hole mass should correlate with the total mass of the galaxies.
Saitoh Takayuki R.
Wada Keiichi
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