Pattern Speed of Lopsidedness in Galactic Disks
| dc.creator | Jog, Chanda J. | |
| dc.date | 2008-12-03 | |
| dc.date.accessioned | 2026-07-07T12:08:44Z | |
| dc.date.available | 2026-07-07T12:08:44Z | |
| dc.description | The disks of spiral galaxies commonly show a lopsided mass distribution, with a typical fractional amplitude of 10 % for the Fourier component m=1. This is seen in both stars and gas, and the amplitude is higher by a factor of two for galaxies in a group. The study of lopsidedness is a new topic, in contrast to the extensively studied bars and two-armed spirals (m=2). Here, first a brief overview of the observations of disk lopsidedness is given, followed by a summary of the various mechanisms that have been proposed to explain its physical origin. These include tidal interactions, gas accretion, and a global instability. The pattern speed of lopsidedness in a real galaxy has not been measured so far, the various issues involved will be discussed. Theoretical studies have shown that the m=1 slow modes are long-lived, while the modes with a moderate pattern speed as triggered in interactions, last for only about a Gyr. Thus a measurement of the pattern speed of lopsided distribution will help identify the mechanism for its origin. | |
| dc.description | 7 pages, 7 figures, Invited review. To appear in "Tumbling, Twisting, and Winding Galaxies: Pattern Speeds along the Hubble Sequence", Padova, Italy, August 2008, E. M. Corsini and V. P. Debattista (eds.), to be published by Memorie della Societa` Astronomica Italiana | |
| dc.identifier | https://arxiv.org/abs/0812.0670 | |
| dc.identifier | http://arxiv.org/abs/0812.0670 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/209426 | |
| dc.subject | Astrophysics | |
| dc.title | Pattern Speed of Lopsidedness in Galactic Disks | |
| dc.type | text |