Stellar metallicity variations across spiral arms in disk galaxies with multiple populations

被引:23
|
作者
Khoperskov, S. [1 ]
Di Matteo, P. [1 ]
Haywood, M. [1 ]
Combes, F. [2 ,3 ]
机构
[1] PSL Univ, CNRS, Observ Paris, GEPI, 5 Pl Jules Janssen, F-92190 Meudon, France
[2] Sorbonne Univ, UPMC, PSL Univ,CNRS, Observ Paris,LERMA, F-75014 Paris, France
[3] Coll France, 11 Pl Marcelin Berthelot, F-75005 Paris, France
基金
俄罗斯基础研究基金会;
关键词
galaxies: evolution; galaxies: kinematics and dynamics; galaxies: structure; VELOCITY DISPERSION; SOLAR NEIGHBORHOOD; STAR-FORMATION; WAVES; MODES; SIGNATURES; MIGRATION; PATTERNS;
D O I
10.1051/0004-6361/201732521
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
This Letter studies the formation of azimuthal metallicity variations in the disks of spiral galaxies in the absence of initial radial metallicity gradients. Using high-resolution N-body simulations, we model composite stellar discs, made of kinematically cold and hot stellar populations, and study their response to spiral arm perturbations. We find that, as expected, disk populations with different kinematics respond differently to a spiral perturbation, with the tendency for dynamically cooler populations to show a larger fractional contribution to spiral arms than dynamically hotter populations. By assuming a relation between kinematics and metallicity, namely the hotter the population, the more metal-poor it is, this differential response to the spiral arm perturbations naturally leads to azimuthal variations in the mean metallicity of stars in the simulated disk. Thus, azimuthal variations in the mean metallicity of stars across a spiral galaxy are not necessarily a consequence of the reshaping, by radial migration, of an initial radial metallicity gradient. They indeed arise naturally also in stellar disks which have initially only a negative vertical metallicity gradient.
引用
收藏
页数:5
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