期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 438, 期 2, 页码 1552-1576出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stt2294
关键词
galaxies: evolution; galaxies: ISM; galaxies: kinematics and dynamics; galaxies: structure
资金
- National Science FoundationAlfred P. Sloan Foundation [DGE0809125, DGE1339067]
- NSF [AST-0955300, AST-1010033]
- NASA
- ATFP [NNX13AB84G]
- GIF [G-1052-104.7/2009]
- ISF [24/12]
- Direct For Mathematical & Physical Scien [0955300] Funding Source: National Science Foundation
- Division Of Astronomical Sciences [0955300] Funding Source: National Science Foundation
Over the past 10 Gyr, star-forming galaxies have changed dramatically, from clumpy and gas rich, to rather quiescent stellar-dominated discs with specific star formation rates lower by factors of a few tens. We present a general theoretical model for how this transition occurs, and what physical processes drive it, making use of 1D axisymmetric thin disc simulations with an improved version of the Gravitational Instability-Dominated Galaxy Evolution Tool (GIDGET) code. We show that at every radius galaxies tend to be in a slowly evolving equilibrium state wherein new accretion is balanced by star formation, galactic winds and radial transport of gas through the disc by gravitational instability-driven torques. The gas surface density profile is determined by which of these terms are in balance at a given radius - direct accretion is balanced by star formation and galactic winds near galactic centres, and by transport at larger radii. We predict that galaxies undergo a smooth transition from a violent disc instability phase to secular evolution. This model provides a natural explanation for the high velocity dispersions and large clumps in z similar to 2 galaxies, the growth and subsequent quenching of bulges, and features of the neutral gas profiles of local spiral galaxies.
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