Impact of bar resonances in the velocity–space distribution of the solar neighbourhood stars in a self-consistent N-body Galactic disc simulation. Issue 1 (19th May 2022)

• Record Type: Journal Article
• Authors: Asano, Tetsuro; Fujii, Michiko S; Baba, Junichi; Bédorf, Jeroen; Sellentin, Elena; Portegies Zwart, Simon
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 514:Issue 1(2022)
• Page Start: 460
• Page End: 469
• Publication Date: 2022-05-19
• Subjects: methods: numerical -- Galaxy: disc -- Galaxy: kinematics and dynamics -- solar neighbourhood -- Galaxy: structure; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stac1379
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: The velocity–space distribution of the solar neighbourhood stars shows complex substructures. Most of the previous studies use static potentials to investigate their origins. Instead we use a self-consistent N -body model of the Milky Way, whose potential is asymmetric and evolves with time. In this paper, we quantitatively evaluate the similarities of the velocity–space distributions in the N -body model and that of the solar neighbourhood, using Kullback–Leibler divergence (KLD). The KLD analysis shows the time evolution and spatial variation of the velocity–space distribution. The KLD fluctuates with time, which indicates the velocity–space distribution at a fixed position is not always similar to that of the solar neighbourhood. Some positions show velocity–space distributions with small KLDs (high similarities) more frequently than others. One of them locates at $(R, \phi)=(8.2\, \, \rm{\mathrm{kpc}}, 30^\circ)$, where R and ϕ are the distance from the galactic centre and the angle with respect to the bar's major axis, respectively. The detection frequency is higher in the inter-arm regions than in the arm regions. In the velocity maps with small KLDs, we identify the velocity–space substructures, which consist of particles trapped in bar resonances. The bar resonances have significant impact on the stellar velocity–space distribution even though the galactic potential is not static.