Self-consistent massive disks in triaxial dark matter halos

被引:22
作者
Bailin, Jeremy
Simon, Joshua D.
Bolatto, Alberto D.
Gibson, Brad K.
Power, Chris
机构
[1] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia
[2] CALTECH, Dept Astron, Pasadena, CA 91125 USA
[3] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA
[4] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA
[5] Univ Cent Lancashire, Ctr Astrophys, Preston PR1 2HE, Lancs, England
关键词
dark matter; galaxies : halos; galaxies : kinematics and dynamics; galaxies : spiral; galaxies : structure; methods : numerical;
D O I
10.1086/520843
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Galactic disks in triaxial dark matter halos become deformed by the elliptical potential in the plane of the disk in such a way as to counteract the halo ellipticity. We develop a technique to calculate the equilibrium configuration of such a disk in the combined disk-halo potential, which is based on the method of Jog but accounts for the radial variation in both the halo potential and the disk ellipticity. This crucial ingredient results in qualitatively different behavior of the disk: the disk circularizes the potential at small radii, even for a reasonably low disk mass. This effect has important implications for proposals to reconcile cuspy halo density profiles with low surface brightness galaxy rotation curves using halo triaxiality. The disk ellipticities in our models are consistent with observational estimates based on two-dimensional velocity fields and isophotal axis ratios.
引用
收藏
页码:191 / 201
页数:11
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