Role of gas in supporting grand spiral structure

• Published in: Monthly notices of the Royal Astronomical Society Vol. 451; no. 2; pp. 1350 - 1355
• Main Authors: Ghosh, Soumavo, Jog, Chanda J.
• Format: Journal Article
• Language: English
• Published: London Oxford University Press 01-08-2015
• Subjects: Astronomical instruments; Cosmology; Density; Discs; Disks; Dispersion; Dispersions; Galaxies; Gases; Protoplanetary disks; Spirals; Star & galaxy formation; Transport; Velocity; galaxies: structure; galaxies: kinematics and dynamics; galaxies: spiral; galaxies: ISM
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1093/mnras/stv1040

The density wave theory for the grand-design two-armed spiral pattern in galaxies
is successful in explaining several observed features. However, the long-term persistence of this spiral structure is a serious problem since the group transport would destroy it within about a billion years as shown in a classic paper by Toomre. In this paper, we include the low-velocity dispersion component, namely gas, on an equal footing with stars in the formulation of the density wave theory, and obtain the dispersion relation for this coupled system. We show that the inclusion of gas makes the group transport slower by a factor of few, thus allowing the pattern to persist longer – for several billion years. Though still less than the Hubble time, this helps in making the spiral structure more long-lived. Further we show that addition of gas is essential to get a stable wave for the observed pattern speed for the Galaxy, which otherwise is not possible for a one-component stellar disc.