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Can Dust Destabilise Galactic Disks?

Published online by Cambridge University Press:  05 March 2013

Christian Theis  and
Natalya Orlova
Christian Theis*
Affiliation:
Institut für Theoretische Physik und Astrophysik der Universität Kiel, 24098 Kiel, Germany
Natalya Orlova
Affiliation:
Institute of Physics, Stachki 194, Rostov-on-Don, Russia
*
4E-mail: [email protected]
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Abstract

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We studied the dynamic influence of a dust component on the gaseous phase in central regions of galactic disks. We performed two-dimensional hydrodynamic simulations for flat, multicomponent disks embedded in a stellar and dark matter potential. The pressure-free dust component is coupled to the gas by a drag force depending on their velocity difference. The most unstable regions are those with either a low or near-to-minimum Toomre parameter or with rigid rotation, i.e. the central area. In those regions the dust-free disks become most unstable for a small range of high azimuthal modes (m ∼ 8), whereas in dusty disks all modes have similar amplitudes resulting in a patchy appearance. The structures in the dust have a larger contrast between arm and interarm regions than those of the gas. The dust peaks are frequently correlated with peaks of the gas distribution, but they do not necessarily coincide with them. This leads to a large scatter in the dust to gas ratios. The appearance of the dust is more cellular (i.e. sometimes connecting different spiral features), whereas the gas is organised in a multi-armed spiral structure. We found that an admixture of 2% dust (relative to the mass of the gas) destabilises gaseous disks substantially, whereas dust to gas ratios below 1% have no influence on the evolution of the gaseous disk. For a high dust to gas ratio of 10% the instabilities reach the saturation level after 30 Myr.

Keywords

galaxies: kinematics and dynamicsgalaxies: spiraldust, extinctionISM: structure
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 21 , Issue 2: The Fifth Workshop on Galactic Chemodynamics , 2004 , pp. 179 - 182
Copyright
Copyright © Astronomical Society of Australia 2004

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