Violent Buckling Benefits Galactic Bars

Abstract

Galactic bars are unstable to a vertical buckling instability which heats the disk and in some cases forms a boxy/peanut shaped bulge. We analyze the buckling instability as an application of classical Euler buckling followed by nonlinear gravitational Landau damping in the collisionless system. We find that the buckling instability is dictated by the kinematic properties and geometry of the bar. The analytical result is compared to simulations of isolated galaxies containing the disk and dark matter components. Our results demonstrate that violent buckling does not destroy bars while a less energetic buckling can dissolve the bar. The disks that undergo gentle buckling remain stable to bar formation which may explain the observed bar fraction in the local universe. Our results align with the results from recent surveys.

9 pages, 7 figures

References in corpus (26)

• The Structure of Cold Dark Matter Halos
• GIZMO: A New Class of Accurate, Mesh-Free Hydrodynamic Simulation Methods
• A universal angular momentum profile for galactic halos
• Morphology, photometry and kinematics of N-body bars. I Three models with different halo central concentrations
• The Secular Evolution of Disk Structural Parameters
• Evolution of Stellar Bars in Live Axisymmetric Halos: Recurrent Buckling and Secular Growth
• Our Milky Way as a Pure-Disk Galaxy -- A Challenge for Galaxy Formation
• The Dependence of Bar Frequency on Galaxy Mass, Colour, and Gas Content -- and Angular Resolution -- in the Local Universe
• Orbital dynamics of three-dimensional bars: I. The backbone of 3D bars. A fiducial case
• Separation of Stellar Populations by an Evolving Bar: Implications for the Bulge of the Milky Way
• Anatomy of the Bar Instability in Cuspy Dark Matter Halos
• Unifying boxy bulge and planar long bar in the Milky Way
• Why Buckling Stellar Bars Weaken in Disk Galaxies
• Spinning dark matter halos promote bar formation
• Hot Disks And Delayed Bar Formation
• An Iterative Method for Constructing Equilibrium Phase Models of Stellar Systems
• What Makes the Family of Barred Disc Galaxies So Rich: Damping Stellar Bars in Spinning Haloes
• Revealing the cosmic evolution of boxy/peanut-shaped bulges from HST COSMOS and SDSS
• Caught in the Act: Direct Detection of Galactic Bars in the Buckling Phase
• Violent Relaxation, Phase Mixing, and Gravitational Landau Damping
• Meridional tilt of the stellar velocity ellipsoid during bar buckling instability
• The structural evolution of galaxies with both thin and thick discs
• Dark Matter Bars in Spinning Halos
• Stellar Bars in Counter-Rotating Dark Matter Halos: The Role of Halo Orbit Reversals
• An Iterative Method for the Construction of Equilibrium N-Body Models for Stellar Disks
• On the Dynamics of the Inclination Instability

Cited by in corpus (18)

• Three Mechanisms for Bar Thickening
• Box/peanut-shaped bulges in action space
• Modeling Evolution of Galactic Bars at Cosmic Dawn
• Can General Relativity play a role in galactic dynamics?
• Effects of Inner Halo Angular Momentum on the Peanut/X-shapes of Bars
• A New Discrete Dynamical Friction Estimator Based on $N$-body Simulations
• The Coupling of Galactic Dark Matter Halos with Stellar Bars
• The Effect of Dark Matter Halo Shape on Bar Buckling and Boxy/Peanut Bulges
• Bar-driven Leading Spiral Arms in a Counter-rotating Dark Matter Halo
• Testing for relics of past strong buckling events in edge-on galaxies: Simulation predictions and data from S${}^4$G
• Predicted Trends in Milky Way Bulge Proper Motion Rotation Curves: future Prospects for HST and LSST
• Early Growing Supermassive Black Holes Strengthen Bars and Boxy/Peanut Bulges
• Dynamical analysis of Maclaurin disk with velocity dispersion and its influence on bar formation
• On the nature of buckling instability in galactic bars
• Intrinsic properties of the bars formed by the bar instability in flat stellar discs
• Bar Evolution in Edge-on Galaxies: A Demographic Study of Boxy/Peanut Bulges
• Numerical Study of Bar Suppression in Galaxy Models Due to Disc Heating
• Age distribution of stars in boxy/peanut/X-shaped bulges formed without bar buckling