Vertical disc heating in Milky Way-sized galaxies in a cosmological context. Issue 1 (15th March 2016)

• Record Type: Journal Article
• Authors: Grand, Robert J. J.; Springel, Volker; Gómez, Facundo A.; Marinacci, Federico; Pakmor, Rüdiger; Campbell, David J. R.; Jenkins, Adrian
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 459:Issue 1(2016)
• Page Start: 199
• Page End: 219
• Publication Date: 2016-03-15
• Subjects: methods: numerical -- galaxies: evolution -- galaxies: formation -- galaxies: kinematics and dynamics -- galaxies: spiral -- galaxies: structure; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stw601
• Languages: English
• ISSNs: 0035-8711

Abstract

Abstract : Vertically extended, high velocity dispersion stellar distributions appear to be a ubiquitous feature of disc galaxies, and both internal and external mechanisms have been proposed to be the major driver of their formation. However, it is unclear to what extent each mechanism can generate such a distribution, which is likely to depend on the assembly history of the galaxy. To this end, we perform 16 high-resolution cosmological-zoom simulations of Milky Way-sized galaxies using the state-of-the-art cosmological magnetohydrodynamical code arepo, and analyse the evolution of the vertical kinematics of the stellar disc in connection with various heating mechanisms. We find that the bar is the dominant heating mechanism in most cases, whereas spiral arms, radial migration and adiabatic heating from mid-plane density growth are all subdominant. The strongest source, though less prevalent than bars, originates from external perturbations from satellites/subhaloes of masses log10 ( M /M⊙ ) ≳ 10. However, in many simulations the orbits of newborn star particles become cooler with time, such that they dominate the shape of the age–velocity dispersion relation and overall vertical disc structure unless a strong external perturbation takes place.