The origin of <i>rR</i><sub>1</sub> ring structures in
barred galaxies

Romero-Gómez, M.; Masdemont, Josep J.; Athanassoula, E.; García-Gómez, C.

doi:10.1051/0004-6361:20054653

Cited by 135 publications

(166 citation statements)

References 34 publications

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“…This is important since the rings and spirals in barred galaxies are observational properties. So we obtain connections between the parameters in our model and observational results (e.g., Athanassoula et al 2009aAthanassoula et al ,b, 2010Athanassoula et al , 2011Romero-Gómez et al 2006, 2007.…”

Section: Introductionsupporting

confidence: 69%

Orbital and escape dynamics in barred galaxies – III. The 3D system: correlations between the basins of escape and the NHIMs

Zotos

Jung

2017

Monthly Notices of the Royal Astronomical Society

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The escape dynamics of the stars in a barred galaxy composed of a spherically symmetric central nucleus, a bar, a flat thin disk and a dark matter halo component is investigated by using a realistic three degrees of freedom (3-dof) dynamical model. Modern colour-coded diagrams are used for distinguishing between bounded and escaping motion. In addition, the smaller alignment index (SALI) method is deployed for determining the regular, sticky or chaotic nature of bounded orbits. We reveal the basins of escape corresponding to the escape through the two symmetrical escape channels around the Lagrange points L 2 and L 3 and also we relate them with the corresponding distribution of the escape times of the orbits. Furthermore, we demonstrate how the stable manifolds, around the index-1 saddle points, accurately define the fractal basin boundaries observed in the colour-coded diagrams. The development scenario of the fundamental vertical Lyapunov periodic orbit is thoroughly explored for obtaining a more complete view of the unfolding of the singular behaviour of the dynamics at the cusp values of the parameters. Finally, we examine how the combination of the most important parameters of the bar (such as the semi-major axis and the angular velocity) influences the observed stellar structures (rings and spirals) which are formed by escaping stars guided by the invariant manifolds near the saddle points.

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Section: Introductionsupporting

confidence: 69%

Orbital and escape dynamics in barred galaxies – III. The 3D system: correlations between the basins of escape and the NHIMs

Zotos

Jung

2017

Monthly Notices of the Royal Astronomical Society

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“…Owing to star formation triggered by the high gas density and by gas travelling in intersecting orbits at each side of the resonance, rings and pseudorings are often formed there (Schwarz 1981(Schwarz , 1984. Historically, this picture has been used to explain resonance rings and pseudorings, but recently an alternative model, called the flux tube manifold theory or manifold theory, postulated that at least some of them are caused by gas and/or stars trapped in tubes of orbits that connect the Lagrangian points at the end of the galaxy bars (Romero-Gómez et al 2006Athanassoula et al 2009bAthanassoula et al ,a, 2010Athanassoula 2012b). Another alternative ring formation mechanism is that developed by Kim et al (2012) for nuclear rings (not studied here), where rings are formed due to the centrifugal barrier encountered by gas migrating to inner regions of the galaxy.…”

Section: Introductionmentioning

confidence: 99%

Inner rings in disc galaxies: dead or alive

Comerón

2013

A&A

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In this Letter, I distinguish "passive" inner rings as those with no current star formation as distinct from "active" inner rings that have undergone recent star formation. I built a sample of nearby galaxies with inner rings observed in the near-and mid-infrared from the NIRS0S and the S 4 G surveys. I used archival far-ultraviolet (FUV) and Hα imaging of 319 galaxies to diagnose whether their inner rings are passive or active. I found that passive rings are found only in early-type disc galaxies (−3 ≤ T ≤ 2). In this range of stages, 21 ± 3% and 28 ± 5% of the rings are passive according to the FUV and Hα indicators, respectively. A ring that is passive according to the FUV is always passive according to Hα, but the reverse is not always true. Ring-lenses form 30-40% of passive rings, which is four times more than the fraction of ring-lenses found in active rings in the stage range −3 ≤ T ≤ 2. This is consistent with both a resonance and a manifold origin for the rings because both models predict purely stellar rings to be wider than their star-forming counterparts. In the case of resonance rings, the widening may be at least partly due to the dissolution of rings. If most inner rings have a resonance origin, I estimate 200 Myr to be a lower bound for their dissolution time-scale. This time-scale is of the order of one orbital period at the radius of inner rings.

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“…It is worth mentioning that there exist several papers where invariant manifolds have been applied in galactic dynamics. In a germinal paper by Romero-Gómez et al (2006), the authors introduce a new theory for the formation of ring structures in barred galaxies. Concretely, they propose that rings are formed by material from the invariant manifolds associated with a type of periodic orbits.…”

Section: Introductionmentioning

confidence: 99%

Tails and bridges in the parabolic restricted three-body problem

Barrabés

Cors

Garcia-Taberner

et al. 2017

Monthly Notices of the Royal Astronomical Society

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After a close encounter of two galaxies, bridges and tails can be seen between or around them. A bridge would be a spiral arm between a galaxy and its companion, whereas a tail would correspond to a long and curving set of debris escaping from the galaxy. The goal of this paper is to present a mechanism, applying techniques of dynamical systems theory, that explains the formation of tails and bridges between galaxies in a simple model, the so-called parabolic restricted three-body problem, i.e. we study the motion of a particle under the gravitational influence of two primaries describing parabolic orbits. The equilibrium points and the final evolutions in this problem are recalled,and we show that the invariant manifolds of the collinear equilibrium points and the ones of the collision manifold explain the formation of bridges and tails. Massive numerical simulations are carried out and their application to recover previous results are also analysed.

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The origin of rR₁ ring structures in barred galaxies

Cited by 135 publications

References 34 publications

Orbital and escape dynamics in barred galaxies – III. The 3D system: correlations between the basins of escape and the NHIMs

Orbital and escape dynamics in barred galaxies – III. The 3D system: correlations between the basins of escape and the NHIMs

Inner rings in disc galaxies: dead or alive

Tails and bridges in the parabolic restricted three-body problem

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The origin of rR1 ring structures in barred galaxies

Cited by 135 publications

References 34 publications

Orbital and escape dynamics in barred galaxies – III. The 3D system: correlations between the basins of escape and the NHIMs

Orbital and escape dynamics in barred galaxies – III. The 3D system: correlations between the basins of escape and the NHIMs

Inner rings in disc galaxies: dead or alive

Tails and bridges in the parabolic restricted three-body problem

Contact Info

Product

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The origin of rR₁ ring structures in barred galaxies