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Cited by 366Astrophysics and Star Formation StudiesGalaxies: Formation, Evolution, PhenomenaAstrophysics and Cosmic Phenomena

The DOI matches its Crossref record; 151 of the 151 references it cites were found in a registry or an index.

The SILCC (SImulating the LifeCycle of molecular Clouds) project – I. Chemical evolution of the supernova-driven ISM

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Walch, S., Girichidis, P., Naab, T., Gatto, A., Glover, S. C. O., Wünsch, R., Klessen, R. S., Clark, P. C., Peters, T., Derigs, D., Baczynski, C.·2015·Monthly Notices of the Royal Astronomical Society
DOI 10.1093/mnras/stv1975
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Abstract

The SILCC (SImulating the Life-Cycle of molecular Clouds) project aims to self-consistently understand the small-scale structure of the interstellar medium (ISM) and its link to galaxy evolution. We simulate the evolution of the multiphase ISM in a (500 pc)2 × ±5 kpc region of a galactic disc, with a gas surface density of |$\Sigma _{_{\rm GAS}} = 10 \;{\rm M}_{\odot }\,{\rm pc}^{-2}$|⁠. The flash 4 simulations include an external potential, self-gravity, magnetic fields, heating and radiative cooling, time-dependent chemistry of H2 and CO considering (self-) shielding, and supernova (SN) feedback but omit shear due to galactic rotation. We explore SN explosions at different rates in high-density regions (peak), in random locations with a Gaussian distribution in the vertical direction (random), in a combination of both (mixed), or clustered in space and time (clus/clus2). Only models with self-gravity and a significant fraction of SNe that explode in low-density gas are in agreement with observations. Without self-gravity and in models with peak driving the formation of H2 is strongly suppressed. For decreasing SN rates, the H2 mass fraction increases significantly from <10 per cent for high SN rates, i.e. 0.5 dex above Kennicutt–Schmidt, to 70–85 per cent for low SN rates, i.e. 0.5 dex below KS. For an intermediate SN rate, clustered driving results in slightly more H2 than random driving due to the more coherent compression of the gas in larger bubbles. Magnetic fields have little impact on the final disc structure but affect the dense gas (n ≳ 10 cm−3) and delay H2 formation. Most of the volume is filled with hot gas (∼80 per cent within ±150 pc). For all but peak driving a vertically expanding warm component of atomic hydrogen indicates a fountain flow. We highlight that individual chemical species populate different ISM phases and cannot be accurately modelled with temperature-/density-based phase cut-offs.

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Show all 150 references

Research works printed but not linked: 12

  1. Dubey A. Reid L. B. Weide K. Antypas K. Ganapathy M. K. Riley K. Sheeler D. Siegal A. 2009. preprint (arXiv:0903.4875). · arXiv
  2. Girichidis P. . MNRAS. 2015. preprint (arXiv:1508.06646) (SILCC2). · arXiv
  3. Glover, 2012, MNRAS, 421, 9
  4. Glover, 2012, MNRAS, 421, 116
  5. Glover, 2010, MNRAS, 404, 2
  6. Habing, 1968, Bull. Astron. Inst. Netherlands, 19, 421
  7. Honma, 1995, A&A, 304, 1
  8. Lee, 1996, A&A, 311, 690
  9. Li M. Ostriker J. P. Cen R. Bryan G. L. Naab T. 2015. preprint (arXiv:1506.07180). · arXiv
  10. Mathis, 1983, A&A, 128, 212
  11. Ossenkopf, 1994, A&A, 291, 943
  12. Vazquez-Semadeni E. 2009. preprint (arXiv:0902.0820). · arXiv

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Metadata

Authors
Walch, S., Girichidis, P., Naab, T., Gatto, A., Glover, S. C. O., Wünsch, R., Klessen, R. S., Clark, P. C., Peters, T., Derigs, D., & Baczynski, C.
Affiliations
  • University of Cologne (DE)
  • Max Planck Institute for Astrophysics (DE)
  • Heidelberg University (DE)
  • Czech Academy of Sciences (CZ)
  • University of California, Santa Cruz (US)
  • Cardiff University (GB)
  • University of Zurich (CH)
Corresponding author
Walch, S.
ORCID
Venue
Monthly Notices of the Royal Astronomical Society
Publisher
Oxford University Press (OUP)
Published
2015-09-18
Volume
454
Issue
1
Pages
246-276
ISSN
  • 0035-8711 (ISSN-L)
  • 1365-2966
DOI
10.1093/mnras/stv1975
OpenAlex
W2144418467
Semantic Scholar
5552a9a34c63503794c25f4389441ea16aab30f2
Cited by
366
References
150
Citations by year
2026: 12 · 2025: 37 · 2024: 40 · 2023: 40 · 2022: 34 · 2021: 28 · 2020: 38 · 2019: 31 · 2018: 29 · 2017: 29 · 2016: 32 · 2015: 16
FWCI
20.10
Type
journal article
Language
en
Open access
Locations
  • Monthly Notices of the Royal Astronomical Society (publishedVersion)
  • Kölner Universitäts PublikationsServer (Universität zu Köln) (publishedVersion)
  • Zurich Open Repository and Archive (University of Zurich) (acceptedVersion, other-oa)
  • arXiv (Cornell University) (submittedVersion)
  • reroDoc Digital Library (submittedVersion)
  • ASEP (submittedVersion, public-domain)
  • ORCA Online Research @Cardiff (Cardiff University) (submittedVersion)
  • HighWire Press Open Archive (submittedVersion)
  • MPG.PuRe (Max Planck Society) (submittedVersion)
  • Zurich Open Repository and Archive (University of Zurich) (submittedVersion, other-oa)
  • arXiv (Cornell University)
  • Zurich Open Repository and Archive (University of Zurich)
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
  • Physical Sciences › Physics and Astronomy › Nuclear and High Energy Physics › Astrophysics and Cosmic Phenomena
Keywords
interstellar medium, supernova feedback, molecular clouds, interstellar chemistry, molecular hydrogen formation, self-gravity, magnetic field, supernova rate, Kennicutt-Schmidt relation, hot gas, Galactic disc, radiative cooling

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