The Secular Evolution of Disk Structural Parameters

Abstract

We present a comprehensive series of $N$-body as well as $N$-body + SPH simulations to study the secular evolution of the structure of disk galaxies. Our simulations are organized in a hierarchy of increasing complexity, ranging from rigid-halo collisionless simulations to fully live simulations with gas and star formation. Comparisons between the different types of simulations allow us to isolate the role of various physical mechanisms. We focus on the evolution of systems expected in a LCDM universe. Our goal is to examine which structural properties of disk galaxies may result from secular evolution rather than from direct hierarchical assembly. In the vertical direction, we find that various mechanisms can lead to heating. The strongest heating occurs during the vertical buckling instability of a bar. Among the consequences of this instability is the formation of peanut-shaped bulges which produce clear kinematic signatures when observed face-on. We find that bars are robust structures that are not destroyed by buckling. They can be destroyed instead by a central mass concentration but we find that this mass needs to be a large fraction of the total mass of the disk. We then study the evolution of stellar surface density profiles showing how angular momentum redistribution leads to increasing central densities and disk scale lengths and to profile breaks at large radii. The breaks in these simulations are in excellent agreement with observed breaks, even when the evolution is purely collisionless. Disk scale-lengths increase even when the total disk angular momentum is conserved; thus mapping halo angular momenta to scale-lengths is non-trivial. [Abridged]

18 pages, 21 figures, in emulateapj format. Published in ApJ. Animation accompanying submission available at http://www.astro.washington.edu/debattis/research/movies/movies.html. This new version corrects minor typos to match the published version. It also includes a figure 15 with new data and a section 7.1 discussing the requirements for SMBH formation from clump instabilities. appeared in ApJ, 645, 209

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• On the nature of buckling instability in galactic bars
• Rediscovering the Milky Way with orbit superposition approach and APOGEE data III. Panoramic view of the bulge
• Exploring the outskirts of the EAGLE disc galaxies
• Orbit-based structural decomposition and stellar population recovery for edge-on barred galaxies
• Radial Migration in Spiral Galaxies
• Discovery of a Barred-Spiral Galaxy at $z_{spec}$ = 3.16 II. The Star Formation History
• A SHARP Look at Quenching and Bulge-Disk Growth in Massive Galaxies at Cosmic Noon
• Resolving the Outer Disks and Halos of Nearby Galaxies
• Boxy/Peanut Bulges: Comparative Analysis of EGIPS Galaxies and TNG50 Models
• Exponential galaxy discs as the quasi-stationary distribution in a Markov chain model simulating stellar scattering
• Baryon-driven decontraction in Milky Way mass haloes
• A family of potential-density pairs for galactic bars
• Bar Evolution in Edge-on Galaxies: A Demographic Study of Boxy/Peanut Bulges
• Age distribution of stars in boxy/peanut/X-shaped bulges formed without bar buckling
• The COMBS Survey -- III. The Chemodynamical Origins of Metal-Poor Bulge Stars
• COSMOS-Web: Galaxy Size and Surface Brightness Evolution at Rest-Frame 1.22 $\mu$m Since $z=3$
• ELMA: ELlipse-based bar MAjor axis estimator
• The stellar mass distribution of S${}^4$G disk galaxies
• Dynamical properties of high-[Mg/Fe] stars in the Milky Way bar region
• Intrinsic properties of the bars formed by the bar instability in flat stellar discs