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Annual Review of Astronomy and Astrophysics

Volume 60, 2022

Spirals in Galaxies

Abstract

Spirals in galaxies have long been thought to be caused by gravitational instability in the stellar component of the disk, but discerning the precise mechanism had proved elusive. Tidal interactions, and perhaps bars, may provoke some spiral responses, but spirals in many galaxies must be self-excited. We survey the relevant observational data and aspects of disk dynamical theory. The origin of the recurring spiral patterns in simulations of isolated disk galaxies has recently become clear, and it is likely that the mechanism is the same in real galaxies, although evidence to confirm this supposition is hard to obtain. As transient spiral activity increases random motion, the patterns must fade over time unless the disk also contains a dissipative gas component. Continuing spiral activity alters the structure of the disks in other ways: reducing metallicity gradients and flattening rotation curves are two of the most significant. The overwhelming majority of spirals in galaxies have two- or three-fold rotational symmetry, indicating that the cool, thin disk component is massive. Spirals in simulations of halo-dominated disks instead manifest many arms and, consequently, do not capture the expected full spiral-driven evolution. We conclude by identifying areas where further work is needed.

Keyword(s): disk galaxies, kinematics and dynamics, structure and evolution
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2022-08-18
2025-06-21
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/content/journals/10.1146/annurev-astro-052920-104505
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Spirals in Galaxies
Annual Review of Astronomy and Astrophysics 60, 73 (2022); https://doi.org/10.1146/annurev-astro-052920-104505
/content/journals/10.1146/annurev-astro-052920-104505
/content/journals/10.1146/annurev-astro-052920-104505
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Supplementary Data

  • Supplemental Video 1. Animation redrawn from Sellwood & Carlberg (2021).

    The top left panel of the animation, which loops back after a short pause, shows the time evolution of the net overdensity of the disk response to two rings at R=2.5R0 and R=4R0 each of three very light disturbance masses that are driven at the local corotation speed. These rings of particles, marked by large dots and each having a mass of 10-4R0V02/G or almost 1000 times the mass of a background disk particle, were added into a simulation of the stable half-mass Mestel disk in which Q=1.5.

    The disk response in the simulation was fitted by two steadily rotating m=3 waves of fixed shape and amplitude that are illustrated in the top panel. The fitted pattern speeds of each of the responses are Ωp,1=0.404 and Ωp,2=0.252, and the principal resonances are marked by circles. As in the animation, distances are in units of R0 and times are in units of R0/V0.

    The top right panel of the animation shows the time evolution of the superposed fitted disturbances, each turning at the fitted rate, that appear as a shearing transient pattern. From time to time, the pattern breaks into two separate spiral segments that quickly rejoin into a more open spiral that winds up again. The similarity of the more intense parts of the disturbances in the top left and top right panels is evident.

    The bottom two panels illustrate the evolution of the logarithmic spiral spectrum in the simulation on the left and the superposed two waves on the right. The abscissa in these panels is tan γ, where γ is the angle between the radius vector and the tangent to the spiral; it is therefore the complement to the pitch angle α. Here one can see a repeating pattern of a peak moving to the right from leading to trailing as the amplitude rises to a maximum near tan γ = +2, followed by a decrease as the spiral begins to wind more tightly.

    This is a clear demonstration that the superposition of two steady disturbances can create the appearance of swing amplification.

    Reference: Sellwood, J. A. & Carlberg, R. G. 2021, MNRAS, 500:5043-5055

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