Nexae in caverna: the secular evolution of disks via collectively excited, transient spiral structure
Sharon E. Meidt, Arjen van der Wel
astro-ph.GA
Submitted: 2026-08-18
Updated: 2026-08-20
Comments: 23 pages, 5 Figures; accepted for publication in A&A
License: http://arxiv.org/licenses/nonexclusive-distrib/1.0/
Terminology
Sources
- The gravitational potential of spiral perturbations I. The 2D (razor-thin) case
- Spiral Structure Diversity in Milky Way Analogs from TNG50: The Role of Gas and Disk Dynamics
- The diverse nature of spiral arms in the Auriga Superstars cosmological hydrodynamic simulations
- Why is the Galactic disk so cool?
- Galactokinetics II: Spiral structure
- On the radial velocity wave in the Galactic disk
- Effects of Resolution and Local Stability on Galactic Disks: I. Multiple Spiral Mode Formation via Swing Amplification
- Spirals in galaxies
- Enhanced rates of stellar radial migration in gas-rich discs at high redshift
Related papers
- Apparent Stability in Self-Gravitating Turbulence and the Evolution of Molecular Clouds
- Two sets of potential-density basis pairs for the study of radial perturbations in collisionless spherical stellar systems
- Constraining reionization-era Ly alpha escape with JELS-MUSE: a highly complete H alpha-selected sample at z about6.1
- Deriving volume density profiles of filaments from observed surface densities
- Little Red Dots and Supermassive Black Hole Seed Formation in Ultralight Dark Matter Halos
- MEGATRON: how the first stars can create an iron metallicity plateau in the smallest dwarf galaxies