How the bar properties affect the induced spiral structure

Abstract

Stellar bars and spiral arms co-exist and co-evolve in most disc galaxies in the local Universe. However, the physical nature of this interaction remains a matter of debate. In this work, we present a set of numerical simulations based on isolated galactic models aimed to explore how the bar properties affect the induced spiral structure. We cover a large combination of bar properties, including the bar length, axial ratio, mass and rotation rate. We use three galactic models describing galaxies with rising, flat and declining rotation curves. We found that the pitch angle best correlates with the bar pattern speed and the spiral amplitude with the bar quadrupole moment. Our results suggest that galaxies with declining rotation curves are the most efficient forming grand design spiral structure, evidenced by spirals with larger amplitude and pitch angle. We also test the effects of the velocity ellipsoid in a subset of simulations. We found that as we increase the radial anisotropy, spirals increase their pitch angle but become less coherent with smaller amplitude.

Accepted for publication in MNRAS. 16 pages, 16 figures

References in corpus (22)

• Dawes Review 4: Spiral Structures in Disc Galaxies
• Hunting for open clusters in \textit{Gaia} DR2: $582$ new OCs in the Galactic disc
• The Dependence of Bar Frequency on Galaxy Mass, Colour, and Gas Content -- and Angular Resolution -- in the Local Universe
• Gas flow models in the Milky Way embedded bars
• The formation of spiral arms and rings in barred galaxies
• On the origin of rR_1 ring structures in barred galaxies
• The effect of radial migration on galactic disks
• Dissecting simulated disc galaxies II: the age-velocity relation
• Effects of Gas on Formation and Evolution of Stellar Bars and Nuclear Rings in Disk Galaxies
• Constraining dark matter halo profiles and galaxy formation models using spiral arm morphology. I. Method outline
• Bars and spirals in tidal interactions with an ensemble of galaxy mass models
• Spiral structure in nearby galaxies II. comparative analysis and conclusions
• Stellar mass distribution of S${}^4$G disk galaxies and signatures of bar-induced secular evolution
• Kinematic clues to bar evolution for galaxies in the local universe: why the fastest rotating bars are rotating most slowly
• Galactic Rings Revisited. I. CVRHS Classifications of 3962 Ringed Galaxies from the Galaxy Zoo 2 Database
• The Mass Profile and Shape of Bars in the Spitzer Survey of Stellar Structure in Galaxies (S4G): Search for an Age Indicator for Bars
• The analysis of realistic Stellar Gaia mock catalogues. I. Red Clump Stars as tracers of the central bar
• SDSS-IV MaNGA: Bar pattern speed estimates with the Tremaine-Weinberg method and their error sources
• Constraints on Radial Migration in Spiral Galaxies - II. Angular momentum distribution and preferential migration
• How do spiral arm contrasts relate to bars, disk breaks and other fundamental galaxy properties?
• The evolution of pitch angles of spiral arms
• The Contribution of Spiral Arms to the Thick Disk along the Hubble Sequence