Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 684, Issue 2, Pages L79-L82Publisher
IOP PUBLISHING LTD
DOI: 10.1086/592231
Keywords
galaxies : evolution; galaxies : spiral; galaxies : stellar content; Galaxy : stellar content; solar neighborhood; stellar dynamics
Categories
Funding
- NSF [PHY 02-05413]
- RCUK Fellowship at the University of Central Lancashire
- Livesey Award
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [0807213] Funding Source: National Science Foundation
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Stars in disks of spiral galaxies are usually assumed to remain roughly at their birth radii. This assumption is built into decades of modeling of the evolution of stellar populations in our own Galaxy and in external systems. We present results from self-consistent high-resolution N-body + smooth particle hydrodynamics simulations of disk formation, in which stars migrate across significant galactocentric distances due to resonant scattering with transient spiral arms, while preserving their circular orbits. We investigate the implications of such migrations for observed stellar populations. Radial migration provides an explanation for the observed flatness and spread in the age-metallicity relation and the relative lack of metal-poor stars in the solar neighborhood. The presence of radial migration also prompts rethinking of interpretations of extragalactic stellar population data, especially for determinations of star formation histories.
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