A new way to locate corotation resonances in spiral galaxies
Citations Over TimeTop 12% of 1993 papers
Abstract
Kinematical information over the entire disk of a spiral galaxy can be used in a new way to locate the position of the corotation resonance. The spiral residual velocity field has a global appearance that is distinctly different inside and outside the corotation resonance radius. Inside the corotation radius, the spiral velocity field shows a single spiral feature (that is, a single approaching-receding "spiral arm" pair). Outside the corotation radius, there are three spiral features (approaching-receding arm pairs). The corotation radius is located where this morphological change occurs. The effect is a consequence of geometric phase. It should apply generally, regardless of the functional form of the velocity perturbation due to a spiral arm, if the spiral structure is wave-based.
Related Papers
- → Spiral structure of the Galaxy Derived from the Hat Creek survey of neutral hydrogen(1970)2 cited
- → Perturbed precessing ellipses as the building blocks of spiral arms in a barred galaxy with two pattern speeds(2022)1 cited
- → Star formation in disk galaxies and its relation with spiral structure in numerical simulations(2022)1 cited
- Study of the Edge and Outer Spiral Structure in the Spiral Galaxy NGC 5248(1995)
- → Perturbed precessing ellipses as the building blocks of spiral arms in a barred galaxy with two pattern speeds(2022)