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Lopsidedness in Disk Galaxies

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Abstract
A lopsided structure is often seen in spiral galaxies. This lopsidedness can be caused by a dynamical instability that occurs in the stellar component of an initially axisymmetric system. The counter-rotation instability can produce a lopsided structure although counter-rotation is only rarely detected in disk galaxies. Therefore we have examined whether lopsided instabilities can be found in fully rotating disks. Models with no net rotation show a strong lopsided mode and a weaker pair of counter-rotating bars. Fully rotating models show a strong two-armed spiral and a weaker one-armed spiral. In the non-rotating models, the m = 1 mode becomes weaker when there is less counter-rotation, while in the rotating models, it becomes stronger.
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Chicago
Dury, Vanessa, Sven De Rijcke, V. P. Debattista, and Herwig Dejonghe. 2008. “Lopsidedness in Disk Galaxies.” In Astronomical Society of the Pacific Conference Series, 396:357–358. San Francisco: Astronomical Society Pacific.
APA
Dury, V., De Rijcke, S., Debattista, V. P., & Dejonghe, H. (2008). Lopsidedness in Disk Galaxies. ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES (Vol. 396, pp. 357–358). Presented at the International Conference on Formation and Evolution of Galaxy Disks, San Francisco: Astronomical Society Pacific.
Vancouver
1.
Dury V, De Rijcke S, Debattista VP, Dejonghe H. Lopsidedness in Disk Galaxies. ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES. San Francisco: Astronomical Society Pacific; 2008. p. 357–8.
MLA
Dury, Vanessa, Sven De Rijcke, V. P. Debattista, et al. “Lopsidedness in Disk Galaxies.” Astronomical Society of the Pacific Conference Series. Vol. 396. San Francisco: Astronomical Society Pacific, 2008. 357–358. Print.
@inproceedings{695159,
  abstract     = {A lopsided structure is often seen in spiral galaxies. This lopsidedness can be caused by a dynamical instability that occurs in the stellar component of an initially axisymmetric system. The counter-rotation instability can produce a lopsided structure although counter-rotation is only rarely detected in disk galaxies. Therefore we have examined whether lopsided instabilities can be found in fully rotating disks. Models with no net rotation show a strong lopsided mode and a weaker pair of counter-rotating bars. Fully rotating models show a strong two-armed spiral and a weaker one-armed spiral. In the non-rotating models, the m = 1 mode becomes weaker when there is less counter-rotation, while in the rotating models, it becomes stronger.},
  author       = {Dury, Vanessa and De Rijcke, Sven and Debattista, V. P. and Dejonghe, Herwig},
  booktitle    = {ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES},
  isbn         = {978-1-58381-662-2},
  issn         = {1050-3390},
  language     = {eng},
  location     = {Rome, Italy},
  pages        = {357--358},
  publisher    = {Astronomical Society Pacific},
  title        = {Lopsidedness in Disk Galaxies},
  volume       = {396},
  year         = {2008},
}

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