Simulating the interstellar medium of galaxies with radiative transfer, non-equilibrium thermochemistry, and dust
Name
1910.14041.pdf
Description
Accepted version
Size
5.56 MB
Format
Adobe PDF
Checksum (MD5)
0b15772401710dcac4572e46e304cce5
Author(s)
Kannan, Rahul
Marinacci, Federico
Vogelsberger, Mark
Sales, Laura V
Torrey, Paul
Springel, Volker
Hernquist, Lars
Date Issued
October 2020
Journal
Monthly Notices of the Royal Astronomical Society
Publisher
Oxford University Press (OUP)
Citation
Kannan, Rahul et al. "Simulating the interstellar medium of galaxies with radiative transfer, non-equilibrium thermochemistry, and dust." Monthly Notices of the Royal Astronomical Society 499, 4 (October 2020): 5732–5748. © 2020 The Author(s)
Version
Author's final manuscript
Abstract
We present a novel framework to self-consistently model the effects of radiation fields, dust physics, and molecular chemistry (H2) in the interstellar medium (ISM) of galaxies. The model combines a state-of-the-art radiation hydrodynamics module with a H and He non-equilibrium thermochemistry module that accounts for H2 coupled to an empirical dust formation and destruction model, all integrated into the new stellar feedback framework SMUGGLE. We test this model on high-resolution isolated Milky-Way (MW) simulations. We show that the effect of radiation feedback on galactic star formation rates is quite modest in low gas surface density galaxies like the MW. The multiphase structure of the ISM, however, is highly dependent on the strength of the interstellar radiation field. We are also able to predict the distribution of H2, that allow us to match the molecular Kennicutt–Schmidt (KS) relation, without calibrating for it. We show that the dust distribution is a complex function of density, temperature, and ionization state of the gas. Our model is also able to match the observed dust temperature distribution in the ISM. Our state-of-the-art model is well-suited for performing next-generation cosmological galaxy formation simulations, which will be able to predict a wide range of resolved (∼10 pc) properties of galaxies.
MIT Department
MIT Kavli Institute for Astrophysics and Space Research
Massachusetts Institute of Technology. Department of Physics
Terms of Use
Creative Commons Attribution-Noncommercial-Share Alike
Persistent DSpace Link
DOI of Published Version
https://doi.org/10.1093/mnras/staa3249
