Bending instability in galactic discs: advocacy of the linear theory

We demonstrate that in N-body simulations of isolated disc galaxies, there is numerical vertical heating which slowly increases the vertical velocity dispersion and the disc thickness. Even for models with over a million particles in a disc, this heating can be significant. Such an effect is just th...

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Bibliographic Details
Published in:Monthly notices of the Royal Astronomical Society 2013-09, Vol.434 (3), p.2373-2379
Main Authors: Rodionov, S. A., Sotnikova, N. Ya
Format: Article
Language:English
Subjects:
Accretion disks
Astrophysics
Computer Science
Heating
Physics
Simulation
Star & galaxy formation
Velocity
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Summary:We demonstrate that in N-body simulations of isolated disc galaxies, there is numerical vertical heating which slowly increases the vertical velocity dispersion and the disc thickness. Even for models with over a million particles in a disc, this heating can be significant. Such an effect is just the same as in numerical experiments by Sellwood. We also show that in a stellar disc, outside a boxy/peanut bulge, if it presents, the saturation level of the bending instability is rather close to the value predicted by the linear theory. We pay attention to the fact that the bending instability develops and decays very fast, so it cannot play any role in secular vertical heating. However, the bending instability defines the minimal value of the ratio between the vertical and radial velocity dispersions σ z /σ R 0.3 (so indirectly the minimal thickness), which stellar discs in real galaxies may have. We demonstrate that observations confirm the last statement.
ISSN:0035-8711
1365-2966
DOI:10.1093/mnras/stt1183