Snap, crackle, pop: Sub-grid supernova feedback in AMR simulations of disc galaxies

Joakim Rosdahl, Joop Schaye, Yohan Dubois, Taysun Kimm, Romain Teyssier

Research output: Contribution to journalArticle

24 Citations (Scopus)

Abstract

We compare five sub-grid models for supernova (SN) feedback in adaptive mesh refinement (AMR) simulations of isolated dwarf and L-star disc galaxies with 20-40 pc resolution. The models are thermal dump, stochastic thermal, 'mechanical' (injecting energy or momentum depending on the resolution), kinetic and delayed cooling feedback. We focus on the ability of each model to suppress star formation and generate outflows. Our highest resolution runs marginally resolve the adiabatic phase of the feedback events, which correspond to 40 SN explosions, and the first three models yield nearly identical results, possibly indicating that kinetic and delayed cooling feedback converge to wrong results. At lower resolution all models differ, with thermal dump feedback becoming inefficient. Thermal dump, stochastic and mechanical feedback generate multiphase outflows with mass loading factors β ≪ 1, which is much lower than observed. For the case of stochastic feedback, we compare to published SPH simulations, and find much lower outflow rates. Kinetic feedback yields fast, hot outflows with β ~ 1, but only if the wind is in effect hydrodynamically decoupled from the disc using a large bubble radius. Delayed cooling generates cold, dense and slow winds with β > 1, but large amounts of gas occupy regions of temperature-density space with short cooling times. We conclude that either our resolution is too low to warrant physically motivated models for SN feedback, that feedback mechanisms other than SNe are important or that other aspects of galaxy evolution, such as star formation, require better treatment.

Original languageEnglish
Pages (from-to)11-33
Number of pages23
JournalMonthly Notices of the Royal Astronomical Society
Volume466
Issue number1
DOIs
Publication statusPublished - 2017 Jan 1

Fingerprint

disk galaxies
supernovae
grids
outflow
cooling
simulation
kinetics
feedback mechanism
star formation
bubble
explosion
momentum
space density
explosions
gas
bubbles
energy
galaxies
stars
temperature

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Rosdahl, Joakim ; Schaye, Joop ; Dubois, Yohan ; Kimm, Taysun ; Teyssier, Romain. / Snap, crackle, pop : Sub-grid supernova feedback in AMR simulations of disc galaxies. In: Monthly Notices of the Royal Astronomical Society. 2017 ; Vol. 466, No. 1. pp. 11-33.
@article{3dd66a1260964aa7919f94139e5fbb81,
title = "Snap, crackle, pop: Sub-grid supernova feedback in AMR simulations of disc galaxies",
abstract = "We compare five sub-grid models for supernova (SN) feedback in adaptive mesh refinement (AMR) simulations of isolated dwarf and L-star disc galaxies with 20-40 pc resolution. The models are thermal dump, stochastic thermal, 'mechanical' (injecting energy or momentum depending on the resolution), kinetic and delayed cooling feedback. We focus on the ability of each model to suppress star formation and generate outflows. Our highest resolution runs marginally resolve the adiabatic phase of the feedback events, which correspond to 40 SN explosions, and the first three models yield nearly identical results, possibly indicating that kinetic and delayed cooling feedback converge to wrong results. At lower resolution all models differ, with thermal dump feedback becoming inefficient. Thermal dump, stochastic and mechanical feedback generate multiphase outflows with mass loading factors β ≪ 1, which is much lower than observed. For the case of stochastic feedback, we compare to published SPH simulations, and find much lower outflow rates. Kinetic feedback yields fast, hot outflows with β ~ 1, but only if the wind is in effect hydrodynamically decoupled from the disc using a large bubble radius. Delayed cooling generates cold, dense and slow winds with β > 1, but large amounts of gas occupy regions of temperature-density space with short cooling times. We conclude that either our resolution is too low to warrant physically motivated models for SN feedback, that feedback mechanisms other than SNe are important or that other aspects of galaxy evolution, such as star formation, require better treatment.",
author = "Joakim Rosdahl and Joop Schaye and Yohan Dubois and Taysun Kimm and Romain Teyssier",
year = "2017",
month = "1",
day = "1",
doi = "10.1093/mnras/stw3034",
language = "English",
volume = "466",
pages = "11--33",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "1",

}

Snap, crackle, pop : Sub-grid supernova feedback in AMR simulations of disc galaxies. / Rosdahl, Joakim; Schaye, Joop; Dubois, Yohan; Kimm, Taysun; Teyssier, Romain.

In: Monthly Notices of the Royal Astronomical Society, Vol. 466, No. 1, 01.01.2017, p. 11-33.

Research output: Contribution to journalArticle

TY - JOUR

T1 - Snap, crackle, pop

T2 - Sub-grid supernova feedback in AMR simulations of disc galaxies

AU - Rosdahl, Joakim

AU - Schaye, Joop

AU - Dubois, Yohan

AU - Kimm, Taysun

AU - Teyssier, Romain

PY - 2017/1/1

Y1 - 2017/1/1

N2 - We compare five sub-grid models for supernova (SN) feedback in adaptive mesh refinement (AMR) simulations of isolated dwarf and L-star disc galaxies with 20-40 pc resolution. The models are thermal dump, stochastic thermal, 'mechanical' (injecting energy or momentum depending on the resolution), kinetic and delayed cooling feedback. We focus on the ability of each model to suppress star formation and generate outflows. Our highest resolution runs marginally resolve the adiabatic phase of the feedback events, which correspond to 40 SN explosions, and the first three models yield nearly identical results, possibly indicating that kinetic and delayed cooling feedback converge to wrong results. At lower resolution all models differ, with thermal dump feedback becoming inefficient. Thermal dump, stochastic and mechanical feedback generate multiphase outflows with mass loading factors β ≪ 1, which is much lower than observed. For the case of stochastic feedback, we compare to published SPH simulations, and find much lower outflow rates. Kinetic feedback yields fast, hot outflows with β ~ 1, but only if the wind is in effect hydrodynamically decoupled from the disc using a large bubble radius. Delayed cooling generates cold, dense and slow winds with β > 1, but large amounts of gas occupy regions of temperature-density space with short cooling times. We conclude that either our resolution is too low to warrant physically motivated models for SN feedback, that feedback mechanisms other than SNe are important or that other aspects of galaxy evolution, such as star formation, require better treatment.

AB - We compare five sub-grid models for supernova (SN) feedback in adaptive mesh refinement (AMR) simulations of isolated dwarf and L-star disc galaxies with 20-40 pc resolution. The models are thermal dump, stochastic thermal, 'mechanical' (injecting energy or momentum depending on the resolution), kinetic and delayed cooling feedback. We focus on the ability of each model to suppress star formation and generate outflows. Our highest resolution runs marginally resolve the adiabatic phase of the feedback events, which correspond to 40 SN explosions, and the first three models yield nearly identical results, possibly indicating that kinetic and delayed cooling feedback converge to wrong results. At lower resolution all models differ, with thermal dump feedback becoming inefficient. Thermal dump, stochastic and mechanical feedback generate multiphase outflows with mass loading factors β ≪ 1, which is much lower than observed. For the case of stochastic feedback, we compare to published SPH simulations, and find much lower outflow rates. Kinetic feedback yields fast, hot outflows with β ~ 1, but only if the wind is in effect hydrodynamically decoupled from the disc using a large bubble radius. Delayed cooling generates cold, dense and slow winds with β > 1, but large amounts of gas occupy regions of temperature-density space with short cooling times. We conclude that either our resolution is too low to warrant physically motivated models for SN feedback, that feedback mechanisms other than SNe are important or that other aspects of galaxy evolution, such as star formation, require better treatment.

UR - http://www.scopus.com/inward/record.url?scp=85018277569&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85018277569&partnerID=8YFLogxK

U2 - 10.1093/mnras/stw3034

DO - 10.1093/mnras/stw3034

M3 - Article

AN - SCOPUS:85018277569

VL - 466

SP - 11

EP - 33

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 1

ER -