NGC 442 |
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NGC 660 |
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M 77 |
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UGC 4261 |
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UGC 4332 |
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NGC 2628 |
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NGC 2685 |
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UGC 4892 |
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UGC 5101 |
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UGC 5119 |
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M 82 |
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NGC 5964 |
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UGC 5485 |
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NGC 3310 |
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*NGC 3384 |
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NGC 3406 NED01 |
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UGC 6182 |
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NGC 5921 |
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NGC 3718 |
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NGC 3998 |
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NGC 4203 |
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NGC 4262 |
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UGC 7388 |
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NGC 4370 |
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UGC07636 |
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*NGC 4643 |
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NGC 4753 |
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NGC 5103 |
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IC 883 |
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M 51a |
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NGC 5544 |
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ARP199 |
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UGC 9562 |
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UGC 9796 |
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PRCD-51 |
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NGC 6028 |
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UGC 10205 |
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NGC 1042 |
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M 77 |
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NGC 2775 |
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*NGC 3184 |
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M 095 |
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M 096 |
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NGC 3631 |
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NGC 3726 |
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NGC 3810 |
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NGC 4030 |
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NGC 4051 |
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NGC 4123 |
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NGC 4242 |
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NGC 4535 |
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M 058 |
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NGC 4618 |
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M 94 |
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NGC 5248 |
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NGC 5334 |
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*NGC5371 |
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M 101 |
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NGC 5474 |
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NGC 5850 |
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NGC2685 |
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NGC2859 |
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NGC3945 |
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NGC4612 |
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UGC 10205 |
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Ring galaxies are believed to form when a compact smaller galaxy plunges through the center of a larger more
diffuse rotating disk galaxy. The galaxy in transit exerts a brief inward pull on the stars of the target galaxy,
which execute radial harmonic oscillations in addition to their initial circular motion. A series of ring waves
forms and propagates through the target disk, as numerical simulations have convincingly demonstrated (e.g., Lynds
& Toomre 1976; Theys & Spiegel 1977). These radially expanding waves are accompanied by a strong burst of star
formation: observed ring galaxies are usually very blue and possess large HII regions (Theys & Spiegel 1976; Jeske
1986). This is the classical ring galaxy II Hz 4 that was modeled by Lynds & Toomre (1976).
Click on any of these images to know the SDSS properties.
Sahar Allam
Last modified: Thu Jun 30 10:32:56 CDT 2005