Simulating galactic dust grain evolution on a moving mesh
Name
1805.04521.pdf
Description
Accepted version
Size
6.4 MB
Format
Adobe PDF
Checksum (MD5)
ece67f9cbab02472e1c08403df71fb7d
Author(s)
McKinnon, Ryan
Vogelsberger, Mark
Torrey, Paul
Marinacci, Federico
Kannan, Rahul
Date Issued
May 2018
Journal
Monthly Notices of the Royal Astronomical Society
Publisher
Oxford University Press (OUP)
Citation
McKinnon, Ryan et al. “Simulating Galactic Dust Grain Evolution on a Moving Mesh.” Monthly Notices of the Royal Astronomical Society 478,3 (August 2018): 2851–86. © 2018 The Authors
Version
Author's final manuscript
Abstract
Interstellar dust is an important component of the galactic ecosystem, playing a key role in multiple galaxy formation processes. We present a novel numerical framework for the dynamics and size evolution of dust grains implemented in the moving-mesh hydrodynamics code AREPO suited for cosmological galaxy formation simulations. We employ a particle-based method for dust subject to dynamical forces including drag and gravity. The drag force is implemented using a second-order semi-implicit integrator and validated using several dusthydrodynamical test problems. Each dust particle has a grain-size distribution, describing the local abundance of grains of different sizes. The grain-size distribution is discretized with a second-order piecewise linear method and evolves in time according to various dust physical processes, including accretion, sputtering, shattering, and coagulation. We present a novel scheme for stochastically forming dust during stellar evolution and new methods for sub-cycling of dust physics time-steps. Using this model, we simulate an isolated disc galaxy to study the impact of dust physical processes that shape the interstellar grain-size distribution. We demonstrate, for example, howdust shattering shifts the grain-size distribution to smaller sizes, resulting in a significant rise of radiation extinction from optical to nearultraviolet wavelengths. Our framework for simulating dust and gas mixtures can readily be extended to account for other dynamical processes relevant in galaxy formation, like magnetohydrodynamics, radiation pressure, and thermochemical processes. Keywords: methods: numerical, dust, extinction, galaxies: evolution, galaxies: ISM
MIT Department
Massachusetts Institute of Technology. Department of Physics
MIT Kavli Institute for Astrophysics and Space Research
Terms of Use
Creative Commons Attribution-Noncommercial-Share Alike
Persistent DSpace Link
DOI of Published Version
https://doi.org/10.1093/mnras/sty1248
