The Hierarchical Formation of the Galactic Disk
arXiv:astro-ph/0405497 · doi:10.1007/978-1-4020-2862-5_54
Abstract
I review the results of recent cosmological simulations of galaxy formation that highlight the importance of satellite accretion in the formation of galactic disks. Tidal debris of disrupted satellites may contribute to the disk component if they are compact enough to survive the decay and circularization of the orbit as dynamical friction brings the satellite into the disk plane. This process may add a small but non-negligible fraction of stars to the thin and thick disks, and reconcile the presence of very old stars with the protracted merging history expected in a hierarchically clustering universe. I discuss various lines of evidence which suggest that this process may have been important during the formation of the Galactic disk.
paper to be read at the "Penetrating Bars through Masks of Cosmic Dust" conference in South Africa
References in corpus (8)
- Simulations of Galaxy Formation in a Lambda CDM Universe II: The Fine Structure of Simulated Galactic Disks
- Simulations of Galaxy Formation in a Lambda CDM Universe I: Dynamical and Photometric Properties of a Simulated Disk Galaxy
- A Low Latitude Halo Stream around the Milky Way
- A dwarf galaxy remnant in Canis Major: the fossil of an in-plane accretion onto the Milky Way
- Abundances for metal-poor stars with accurate parallaxes I. Basic data
- The Hierarchical Origin of Galaxy Morphologies
- Deciphering The Last Major Invasion of the Milky Way Galaxy
- On the nature of the ring-like structure in the outer Galactic disk