Riding the Spiral Waves: Implications of Stellar Migration for the Properties of Galactic Disks

Simple item page
dc.creatorRoškar, Rok
dc.creatorDebattista, Victor P.
dc.creatorQuinn, Thomas R.
dc.creatorStinson, Gregory S.
dc.creatorWadsley, James
dc.date2008-08-01
dc.date.accessioned2026-07-07T10:01:13Z
dc.date.available2026-07-07T10:01:13Z
dc.descriptionStars in disks of spiral galaxies are usually assumed to remain roughly at their birth radii. This assumption is built into decades of modelling 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 extra-galactic stellar population data, especially for determinations of star formation histories.
dc.description4 pages, 3 figures; Accepted for publication in ApJL
dc.identifierhttps://arxiv.org/abs/0808.0206
dc.identifierhttp://arxiv.org/abs/0808.0206
dc.identifier2008, ApJL 684, L79
dc.identifierdoi:10.1086/592231
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/168558
dc.subjectAstrophysics
dc.titleRiding the Spiral Waves: Implications of Stellar Migration for the Properties of Galactic Disks
dc.typetext

Files

Collections

arXiv