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Effects of Gas on Formation and Evolution of Stellar Bars and Nuclear Rings in Disk Galaxies

  • Authors: Woo-Young Seo, Woong-Tae Kim, SungWon Kwak, Pei-Ying Hsieh, Cheongho Han, and Phil F. Hopkins

2019 The Astrophysical Journal 872 5.

  • Provider: AAS Journals

Caption: Figure 8.

Contours of the normalized cross-correlation of the perturbed surface density in the radius-angular frequency plane for models C05 (left) and W05 (right) at different epochs. The solid and dashed lines in each panel plot instantaneous ﹩{\rm{\Omega }}(R)﹩ and ﹩{\rm{\Omega }}\pm \kappa /2﹩. While the pattern speed ﹩{{\rm{\Omega }}}_{b}﹩ of the bars is almost independent of R, corresponding to rigid-body rotation, the pattern speed of the spirals arms is close to Ω at early time and gradually becomes similar to the bar pattern speed at late time. The color bar labels ﹩C(R,\theta ,t)/C(R,{\theta }_{\max },t)﹩.

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