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The existence and shapes of dust lanes in galactic bars
Abstract
I study the flow of gas in and around the bars or ovals of model barred galaxies and show that it is intimately linked to the properties of the periodic orbits. Simulations show that the density of the gas in and around the bar region is low, except for the centre and two narrow lanes which are the loci of shocks. Such shocks form if the x1 periodic orbits have either loops or large curvature values at their apocentres. The form of the shock loci depends on a number of parameters characterizing the bar and disc potentials. In order for shocks to be offset from the bar major axis towards its leading side, the x2 and x3 families must not only exist but also cover a sufficient extent along the bar major axis. The shapes of the shock loci are then understood by the gradual shift of the orientation of the flow lines from that of the x1 orbits to that of x2. Along the shock there is also substantial shear, opposing star formation. The existence of offset shock loci of the observed shape puts strict constraints on the values the various model parameters may take. This should be most useful for deriving bar parameters for observed galaxies. For example, the Lagrangian radius has to lie in the interval (1.2 ± 0.2)a, where a is the length of the bar semimajor axis. For low values of the bar axial ratio or the bar quadrupole moment the shock loci are curved, with their concave sides towards the bar major axis. Substantial inflow is found in models with strong shocks.
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“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 Athanassoula 1992
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Weiner, B. J., & Sellwood, J. A. (1996) · Springer eBooks · doi:10.1007/978-94-009-1687-6_18
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Heller, C. H., & Shlosman, I. (1996) · International Astronomical Union Colloquium · doi:10.1017/s0252921100050235
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Self-citationBar Formation, Evolution and Destruction
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“In most cases, we associate dust lanes with shocks in the gas ow and then appeal to hydrodynamical simulations (Athanassoula 1992; Weiner, Sellwood & Williams this meeting) which require a fast bar to set up a similar ow pattern.”
BackgroundNeutral Hydrogen in the Bar of NGC 4151
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Metadata
- Authors
- Athanassoula, E.
- Corresponding author
- Athanassoula, E.
- ORCID
- Athanassoula, E.
- Venue
- Monthly Notices of the Royal Astronomical Society
- Publisher
- Oxford University Press (OUP)
- Published
- 1992-11-15
- Volume
- 259
- Issue
- 2
- Pages
- 345-364
- ISSN
- 0035-8711 (ISSN-L)
- 1365-2966
- OpenAlex
- W2050371636
- Cited by
- 1,011
- References
- 0
- Citations by year
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- FWCI
- 6.58
- Type
- journal article
- Language
- en
- Open access
- closed
- Locations
- Monthly Notices of the Royal Astronomical Society (publishedVersion)
- 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
- galactic bars, dust lanes, periodic orbits, shock, gas flow, shear, star formation, barred galaxies, gas inflow
About these checks
Registry, retraction, Cites and statistics results are computed, not judged, with one exception: a printed reference that no index lists is read once by a model before it counts as a citation error. Claims are extracted by a model and kept only when their quote appears verbatim in the text; each cited source is then checked, with a model’s help, for whether it says what the claim relies on. Those verdicts can be wrong — read the claim’s quote and the cited source before relying on one.
Statistics and arithmetic are recomputed, not judged.
Confidence bands are shown only for fields calibrated on our annotated test set. None is calibrated yet, so no band is shown.
What counts as a claim ›How we measure confidence ›How we check this ›
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