Spiral arm pitch angle and galactic shear rate in N-body simulations of disc galaxies

TL;DR

This study uses N-body simulations to confirm that higher galactic shear rates lead to more tightly wound spiral arms, aligning with observational correlations and explaining morphological differences among spiral galaxies.

Contribution

First simulation-based analysis demonstrating the correlation between spiral arm pitch angle and galactic shear rate in N-body models.

Findings

Higher shear rates produce more tightly wound spiral arms.

Overall spiral winding increases over time, contributing to observed scatter.

Simulation results align with observational trends in galaxy morphology.

Abstract

Spiral galaxies are observed to exhibit a range of morphologies, in particular in the shape of spiral arms. A key diagnostic parameter is the pitch angle, which describes how tightly wound the spiral arms are. Observationally and analytically, a correlation between pitch angle and galactic shear rate has been detected. For the first time, we examine whether this effect is detected in N-body simulations by calculating and comparing pitch angles of both individual density waves and overall spiral structure in a suite of N-body simulations. We find that higher galactic shear rates produce more tightly wound spiral arms, both in individual mode patterns (density waves) and in the overall density enhancement. Although the mode pattern pitch angles by construction remain constant with time, the overall logarithmic spiral arm winds over time, which could help to explain the scatter in the relation between pitch angle versus shear seen from observations. The correlation between spiral arm pitch angle and galactic shear rate that we find in N-body simulations may also explain why late Hubble type of spiral galaxies tend to have more open arms.