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Cited by 127Galaxies: Formation, Evolution, PhenomenaStellar, planetary, and galactic studiesAstrophysical Phenomena and Observations

Gas flow in barred potentials

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Sormani, Mattia C., Binney, James, Magorrian, John·2015·Monthly Notices of the Royal Astronomical Society
DOI 10.1093/mnras/stv441
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Abstract

We use a Cartesian grid to simulate the flow of gas in a barred Galactic potential and investigate the effects of varying the sound speed in the gas and the resolution of the grid. For all sound speeds and resolutions, streamlines closely follow closed orbits at large and small radii. At intermediate radii shocks arise and the streamlines shift between two families of closed orbits. The point at which the shocks appear and the streamlines shift between orbit families depends strongly on sound speed and resolution. For sufficiently large values of these two parameters, the transfer happens at the cusped orbit as hypothesized by Binney et al. over two decades ago. For sufficiently high resolutions, the flow downstream of the shocks becomes unsteady. If this unsteadiness is physical, as appears to be the case, it provides a promising explanation for the asymmetry in the observed distribution of CO.

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  • Gas undergoes a shock at the intersection of x1 orbits and loses angular momentum, then flows toward the center and settles into a ring-like structure closely following the x2 orbits, forming CMZ-like rings in galaxies.

    “While an intersecting set of orbits can remain stable in a collisionless system, the gas undergoes a shock at the intersection and loses angular momentum. The gas then flows towards the center and finally settles into a ring-like structure closely following the x 2 orbits and thus forming the CMZ-like rings in galaxies (Binney et al. 1991; Athanassoula 1992; Sormani et al. 2015).”

    From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Sormani et al. 2015

    The Results (p. 3) show gas following outer x1 orbits, passing through shocks, and plunging into a central x2 disc identified with the central molecular zone. The paper does not explicitly say that the gas loses angular momentum at an orbit intersection or that this process forms CMZ-like rings across galaxies. Its Conclusion (p. 15) also says the shock location depends on sound speed and resolution, rather than always occurring where x1 orbits become self-intersecting. (LLM, conf=0.84)

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Research works printed but not linked: 7

  1. Binney J., Merrifield M., 1998, Galactic Astronomy. Princeton University Press
  2. Combes F., 1996, in Buta R., Crocker D. A., Elmegreen B. G., eds, Astronomical Society of the Pacific Conference Series Vol. 91, IAU Colloq. 157: Barred Galaxies. p. 286
  3. Hanawa T., Kikuchi D., 2012, in Pogorelov N. V., Font J. A., Audit E., Zank G. P., eds, Astronomical Society of the Pacific Conference Series Vol. 459, Numerical Modeling of Space Plasma Slows (ASTRONUM 2011). p. 310
  4. Maciejewski W., 2008, in Bureau M., Athanassoula E., Barbuy B., eds, IAU Symposium Vol. 245, IAU Symposium. pp 161-164
  5. Roe P. L., 1986, Annual Review of Fluid Mechanics, 18, 337
  6. Sod G. A., 1978, Journal of Computational Physics, 27, 1
  7. van Leer B., 1977, Journal of Computational Physics, 23, 263 Wada K., Koda J., 2004, MNRAS, 349, 270

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Authors
Sormani, M. C., Binney, J., & Magorrian, J.
Affiliations
  • University of Oxford (GB)
  • Institut d'Astrophysique de Paris (FR)
Corresponding author
Sormani, Mattia C.
ORCID
Venue
Monthly Notices of the Royal Astronomical Society
Publisher
Oxford University Press (OUP)
Published
2015-04-01
Volume
449
Issue
3
Pages
2421-2435
ISSN
  • 0035-8711 (ISSN-L)
  • 1365-2966
DOI
10.1093/mnras/stv441
OpenAlex
W2048167658
Cited by
127
References
31
Citations by year
2026: 7 · 2025: 14 · 2024: 16 · 2023: 11 · 2022: 10 · 2021: 12 · 2020: 19 · 2019: 8 · 2018: 9 · 2017: 5 · 2016: 8 · 2015: 8
FWCI
5.69
Type
journal article
Language
en
Open access
Locations
  • Monthly Notices of the Royal Astronomical Society (publishedVersion)
  • arXiv (Cornell University) (submittedVersion)
  • HAL (submittedVersion, other-oa)
  • IrInSubria (University of Insubria) (submittedVersion)
  • arXiv (Cornell University)
Funders
Science and Technology Facilities Council (ST/J00149X/1, PP/D001242/1, ST/I001077/1, ST/K00106X/1, ST/G002479/1)
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysical Phenomena and Observations
Keywords
barred galaxies, gas flow, sound velocity, shock, periodic orbits, orbital families, unsteady flow, grid resolution effects, galactic bars

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