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6.4. Formation and evolution of gaseous bars

Published online by Cambridge University Press:  25 May 2016

D. Friedli
D. Friedli*
Affiliation:
Université Laval and Observatoire du Mt-Mégantic, Québec, QC, G1K 7P4, Canada. dfriedli@phy.ulaval.ca

Extract

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Although numerous gaseous bars are observed, they seem to be much less common than stellar bars. This might be due to an observational bias, but gaseous bars could also be difficult to form and/or have short lifetimes. Gas morphology is strongly dependent on the resolution and the considered scale. A true bar-like shape (Maffei 2) should not be confused with either ring-like plus open arms (IC 342), or “twin peaks” (NGC 3351) morphologies. Typical observed gaseous bar characteristics are 2ag ~ 1 kpc, and Mg ~ 0.1–0.3Mdyn inside a few 100 pc. Below, three mechanisms of gaseous bar formation, as well as their evolution, are briefly discussed.

Type
Part II. Nuclear Interstellar Medium
Information
Symposium - International Astronomical Union , Volume 184: The Central Regions of the Galaxy and Galaxies , 1998 , pp. 269 - 270
Copyright
Copyright © Kluwer 1998 

References

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