Gas accretion in disk galaxies
arXiv:1309.1603
Abstract
Gas accretion is necessary to maintain star formation, spiral and bar structure, and secular evolution in galaxies. This can occur through tidal interaction, or mass accretion from cosmic filaments. Different processes will be reviewed to drive gas towards galaxy centers and trigger starbursts and AGN. The efficiency of these dynamical processes can be estimated through simulations and checked by observations at different redshift, across the Hubble time. Large progress has been made on galaxies at moderate and high redshifts, allowing to interpret the star formation history and star formation efficiency as a function of gas content, dynamical state and galaxy evolution.
10 pages, 4 figures, Arkansas Conference, Structure and Dynamics of Disk Galaxies, M. Seigar and P.Treuthardt, eds
Cited by in corpus (5)
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- The Diversity of Thick Galactic Discs
- The imprint of the thick stellar disc in the mid-plane of three early-type edge-on galaxies in the Fornax cluster
- Dwarf irregular galaxies with extended HI gas disks: Suppression of small-scale spiral structure by dark matter halo
- Cosmic evolution of gas content and accretion