Self-consistent response of a galactic disc to vertical perturbations

Details Self-consistent response of a galactic disc to vertical perturbations Self-consistent response of a galactic disc to vertical perturbations

2006-01-08

arxiv.org/abs/astro-ph/0601160v1

Mon.Not.Roy.Astron.Soc. 367 (2006) 1297-1307

Astronomy and Astrophysics

Astrophysics

10 pages, 5 figures, accepted for publication in MNRAS

Scientific paper

10.1111/j.1365-2966.2006.10045.x

We study the self-consistent, linear response of a galactic disc to vertical perturbations as induced say by a tidal interaction. We calculate the self-gravitational potential corresponding to a non-axisymmetric, self-consistent density response of the disc using the Green's function method. The response potential is shown to oppose the perturbation potential because the self-gravity of the disc resists the imposed potential, and this resistence is stronger in the inner parts of a galactic disc. For the m=1 azimuthal wavenumber, the disc response opposes the imposed perturbation upto a radius that spans a range of 4-6 disc scale-lengths, so that the disc shows a net warp only beyond this region. This physically explains the well-known but so far unexplained observation (Briggs 1990) that warps typically set in beyond this range of radii. We show that the inclusion of a dark matter halo in the calculation only marginally changes (by ~ 10 %) the radius for the onset of warps. For perturbations with higher azimuthal wavenumbers, the net signature of the vertical perturbations can only be seen at larger radii - for example beyond 7 exponential disc scale-lengths for m=10. Also, for high m cases, the magnitude of the negative disc response due to the disc self-gravity is much smaller. This is shown to result in corrugations of the mid-plane density, which explains the puzzling scalloping with m=10 detected in HI in the outermost regions ~ 30 kpc in the Galaxy by Kulkarni et al. (1982).

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