A dynamical mechanism for the origin of nuclear rings

• Published in: Monthly notices of the Royal Astronomical Society Vol. 481; no. 1; pp. 2 - 19
• Main Authors: Sormani, Mattia C, Sobacchi, Emanuele, Fragkoudi, Francesca, Ridley, Matthew, Treß, Robin G, Glover, Simon C O, Klessen, Ralf S
• Format: Journal Article
• Language: English
• Published: Oxford University Press (OUP): Policy P - Oxford Open Option A 21.11.2018
• Subjects: Astrophysics; Physics; galaxies: nuclei; ISM: kinematics and dynamics; galaxies: kinematics and dynamics
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1093/mnras/sty2246

We develop a dynamical theory for the origin of nuclear rings in barred galaxies. In analogy with the standard theory of accretion discs, our theory is based on shear viscous forces among nested annuli of gas. However, the fact that gas follows non-circular orbits in an external barred potential has profound consequences: it creates a region of reverse shear in which it is energetically favourable to form a stable ring that does not spread despite dissipation. Our theory allows us to approximately predict the size of the ring given the underlying gravitational potential. The size of the ring is loosely related to the location of the Inner Lindblad Resonance in the epicyclic approximation, but the predicted location is more accurate and is also valid for strongly barred potentials. By comparing analytical predictions with the results of hydrodynamical simulations, we find that our theory provides a viable mechanism for ring formation if the effective sound speed of the gas is low (c_s≲ 1 {km s^{-1}}), but that nuclear spirals/shocks created by pressure destroy the ring when the sound speed is high (c_s˜eq 10 {km s^{-1}}). We conclude that whether this mechanism for ring formation is relevant for real galaxies ultimately depends on the effective equation of state of the interstellar medium (ISM). Promising confirmation comes from simulations in which the ISM is modelled using state-of-the-art cooling functions coupled to live chemical networks, but more tests are needed regarding the role of turbulence driven by stellar feedback. If the mechanism is relevant in real galaxies, it could provide a powerful tool to constrain the gravitational potential, in particular the bar pattern speed.