Results 101 to 110 of about 7,649 (143)
The Astrophysical Journal, 1983 Spiral arm classifications were made for 261 low-inclination galaxies in groups listed by Huchra and Geller. The fractional occurrence of grand design spiral structure in nonbarred galaxies was found to increase from approx.0.1 to approx.0.6 and then level off as the group crossing rate or galaxy collision rate in a group increases.
Bruce G. Elmegreen, D. M. Elmegreen
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Evidence for small halos in grand design spiral galaxies
The Astrophysical Journal, 1990 Les courbes de rotation de 41 galaxies spirales de differents types sont comparees. Il est montre que les galaxies ayant deux bras longs et symetriques tendent a avoir des courbes de rotation exterieures tombantes alors que les galaxies ayant des bras multiples ou des bras floconneux courts ont plutot des courbes de rotation presques plates ou s ...
D. M. Elmegreen, Bruce G. Elmegreen
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Molecules in galaxies. V - CO observations of flocculent and grand-design spirals
The Astrophysical Journal, 1987 New carbon monoxide (1-0) observations of 29 spiral galaxies are presented and combined with previously existing data for 74 galaxies in order to study the dependence of the average CO surface brightness on the spiral-arm class. The total sample shows no significant correlation between the CO surface brightness and the presence or absence of grand ...
A. A. Stark +2 more
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Grand Design, Multiple Arm, and Flocculent Spiral Galaxies
Annals of the New York Academy of Sciences, 1990 Les proprietes et les origines possibles de 3 types de structure spirale galactique sont passees en ...
Bruce G. Elmegreen
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Observational Manifestation of Chaos in the Gaseous Disk of the Grand Design Spiral Galaxy NGC 3631
Space Science Reviews, 2002 The main goal of the paper is to demonstrate the presence of chaotic trajectories in the gaseous disk of a real spiral galaxy. As an example we have chosen NGC 3631. First, we show the stationarity of the 3-D velocity field restored from the observed line-of-sight velocity field of the gaseous disk.
A. M. Fridman +2 more
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