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INFERNO : Galactic winds in dwarf galaxies with star-by-star simulations including runaway stars

Andersson, Eric P. LU ; Agertz, Oscar LU ; Renaud, Florent LU and Teyssier, Romain (2023) In Monthly Notices of the Royal Astronomical Society 521(2). p.2196-2214
Abstract

The formation and evolution of galaxies have proved sensitive to the inclusion of stellar feedback, which is therefore crucial to any successful galaxy model. We present INFERNO, a new model for hydrodynamic simulations of galaxies, which incorporates resolved stellar objects with star-by-star calculations of when and where the injection of enriched material, momentum, and energy takes place. INFERNO treats early stellar kinematics to include phenomena such as walkaway and runaway stars. We employ this innovative model on simulations of a dwarf galaxy and demonstrate that our physically motivated stellar feedback model can drive vigorous galactic winds. This is quantified by mass and metal loading factors in the range of 10–100, and an... (More)

The formation and evolution of galaxies have proved sensitive to the inclusion of stellar feedback, which is therefore crucial to any successful galaxy model. We present INFERNO, a new model for hydrodynamic simulations of galaxies, which incorporates resolved stellar objects with star-by-star calculations of when and where the injection of enriched material, momentum, and energy takes place. INFERNO treats early stellar kinematics to include phenomena such as walkaway and runaway stars. We employ this innovative model on simulations of a dwarf galaxy and demonstrate that our physically motivated stellar feedback model can drive vigorous galactic winds. This is quantified by mass and metal loading factors in the range of 10–100, and an energy loading factor close to unity. Outflows are established close to the disc, are highly multiphase, spanning almost 8 orders of magnitude in temperature, and with a clear dichotomy between mass ejected in cold, slow-moving (T ≲ 5 × 104 K, v < 100 km s-1) gas and energy ejected in hot, fast-moving (T > 106 K, v > 100 km s-1) gas. In contrast to massive disc galaxies, we find a surprisingly weak impact of the early stellar kinematics, with runaway stars having little to no effect on our results, despite exploding in diffuse gas outside the dense star-forming gas, as well as outside the galactic disc entirely. We demonstrate that this weak impact in dwarf galaxies stems from a combination of strong feedback and a porous interstellar medium, which obscure any unique signatures that runaway stars provide.

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author
; ; and
organization
publishing date
type
Contribution to journal
publication status
published
subject
keywords
galaxies: evolution, ISM: jets, methods: numerical, outflows
in
Monthly Notices of the Royal Astronomical Society
volume
521
issue
2
pages
19 pages
publisher
Oxford University Press
external identifiers
  • scopus:85159800527
ISSN
0035-8711
DOI
10.1093/mnras/stad692
language
English
LU publication?
yes
id
a3f07077-a8e7-4f22-a9ae-c0925aaccd89
date added to LUP
2023-08-23 13:57:52
date last changed
2023-08-23 13:57:52
@article{a3f07077-a8e7-4f22-a9ae-c0925aaccd89,
  abstract     = {{<p>The formation and evolution of galaxies have proved sensitive to the inclusion of stellar feedback, which is therefore crucial to any successful galaxy model. We present INFERNO, a new model for hydrodynamic simulations of galaxies, which incorporates resolved stellar objects with star-by-star calculations of when and where the injection of enriched material, momentum, and energy takes place. INFERNO treats early stellar kinematics to include phenomena such as walkaway and runaway stars. We employ this innovative model on simulations of a dwarf galaxy and demonstrate that our physically motivated stellar feedback model can drive vigorous galactic winds. This is quantified by mass and metal loading factors in the range of 10–100, and an energy loading factor close to unity. Outflows are established close to the disc, are highly multiphase, spanning almost 8 orders of magnitude in temperature, and with a clear dichotomy between mass ejected in cold, slow-moving (T ≲ 5 × 10<sup>4</sup> K, v &lt; 100 km s<sup>-1</sup>) gas and energy ejected in hot, fast-moving (T &gt; 10<sup>6</sup> K, v &gt; 100 km s<sup>-1</sup>) gas. In contrast to massive disc galaxies, we find a surprisingly weak impact of the early stellar kinematics, with runaway stars having little to no effect on our results, despite exploding in diffuse gas outside the dense star-forming gas, as well as outside the galactic disc entirely. We demonstrate that this weak impact in dwarf galaxies stems from a combination of strong feedback and a porous interstellar medium, which obscure any unique signatures that runaway stars provide.</p>}},
  author       = {{Andersson, Eric P. and Agertz, Oscar and Renaud, Florent and Teyssier, Romain}},
  issn         = {{0035-8711}},
  keywords     = {{galaxies: evolution; ISM: jets; methods: numerical; outflows}},
  language     = {{eng}},
  month        = {{05}},
  number       = {{2}},
  pages        = {{2196--2214}},
  publisher    = {{Oxford University Press}},
  series       = {{Monthly Notices of the Royal Astronomical Society}},
  title        = {{INFERNO : Galactic winds in dwarf galaxies with star-by-star simulations including runaway stars}},
  url          = {{http://dx.doi.org/10.1093/mnras/stad692}},
  doi          = {{10.1093/mnras/stad692}},
  volume       = {{521}},
  year         = {{2023}},
}