A<i>Hubble Space Telescope</i>Study of Star Formation in the Inner Resonance Ring of NGC 3081

Buta, Ronald J.; Byrd, G. G.; Freeman, T.

doi:10.1086/382239

Cited by 30 publications

(33 citation statements)

References 56 publications

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“…The brightness profiles of the lenses measured in Kormendy & Bender (2012) are well fitted by Sérsic (1968) functions with n ≃ 0.5 (i. e., Gaussians). (d) When bars and lenses occur together, the bar almost always fills the lens in one dimension (Kormendy 1979bButa 2011Buta , 2012Fig. 1.17 and references there).…”

Section: Bar Suicide and The Origin Of Lens Components II Observationsmentioning

confidence: 99%

“…The properties of inner and outer rings are discussed (for example) in Kormendy (1979bKormendy ( , 1981Kormendy ( , 1982b, Buta (1990Buta ( , 1995Buta ( , 2011Buta ( , 2012, Buta & Crocker (1991), Buta & Combes (1996) and Buta et al (2007). I particularly use the following.…”

Section: Inner Rings "(R)" and Outer Rings "(R)"mentioning

confidence: 99%

“…A lens and an inner ring of the same size can occur together (e. g., NGC 3081). The properties of lenses are established in Kormendy (1979b) and in Buta (2011Buta ( , 2012; Buta et al (1996Buta et al ( , 2007.…”

Section: Lens Components "(Lens)"mentioning

confidence: 99%

“…I will continue to use this notation throughout this review, but I want to make it clear that I believe that (lens) and (oval) structures are fundamentally the same. (4) There also is a continuity from complete outer rings (R) such as the one in NGC 2859 through spiral arms that are distorted until they almost closed to form what is called a "pseudoring" (R ′ ) as in NGC 3504 through to spiral arms that are less -but similarly -distorted as in NGC 4151 ( (1991: RC3) and Buta (2011Buta ( , 2012 for further discussion.…”

Section: Oval Disksmentioning

confidence: 99%

“…Figure 1.44 shows examples of nuclear bars at the centers of barred and oval galaxies. Nuclear bars are well known phenomena (de Vaucouleurs 1959;Sandage 1961;Kormendy 1981Kormendy , 1982bButa et al 2007;Buta 2011Buta , 2012. They are always much smaller than the main bars in which they are embedded.…”

Section: Fundamental Plane Parameter Correlationsmentioning

confidence: 99%

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Secular evolution in disk galaxies

Kormendy¹

2013

Secular Evolution of Galaxies

124

138

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Self-gravitating systems evolve toward the most tightly bound configuration that is reachable via the evolution processes that are available to them. They do this by spreading -the inner parts shrink while the outer parts expand -provided that some physical process efficiently transports energy or angular momentum outward. The reason is that self-gravitating systems have negative specific heats. As a result, the evolution of stars, star clusters, protostellar and protoplanetary disks, black hole accretion disks and galaxy disks are fundamentally similar. How evolution proceeds then depends on the evolution processes that are available to each kind of self-gravitating system. These processes and their consequences for galaxy disks are the subjects of my lectures and of this Canary Islands Winter School.I begin with a review of the formation, growth and death of bars. Then I review the slow ("secular") rearrangement of energy, angular momentum, and mass that results from interactions between stars or gas clouds and collective phenomena such as bars, oval disks, spiral structure and triaxial dark halos. The "existence-proof" phase of this work is largely over: we have a good heuristic understanding of how nonaxisymmetric structures rearrange disk gas into outer rings, inner rings and stuff dumped onto the center. The results of simulations correspond closely to the morphology of barred and oval galaxies. Gas that is transported to small radii reaches high densities. Observations confirm that many barred and oval galaxies have dense central concentrations of gas and star formation. The result is to grow, on timescales of a few Gyr, dense central components that are frequently mistaken for classical (elliptical-galaxy-like) bulges but that were grown slowly out of the disk (not made rapidly by major mergers). The resulting picture of secular galaxy evolution accounts for the richness observed in galaxy structure.

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Section: Bar Suicide and The Origin Of Lens Components II Observationsmentioning

confidence: 99%

Section: Inner Rings "(R)" and Outer Rings "(R)"mentioning

confidence: 99%

Section: Lens Components "(Lens)"mentioning

confidence: 99%

Section: Oval Disksmentioning

confidence: 99%

Section: Fundamental Plane Parameter Correlationsmentioning

confidence: 99%

See 3 more Smart Citations

Secular evolution in disk galaxies

Kormendy¹

2013

Secular Evolution of Galaxies

124

138

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The Classification of Galaxies

Buta

2021

Galaxies

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Origin of the Cartwheel Galaxy: Disk Instability?

Griv

2005

Astrophys Space Sci

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The linear theory and N -body simulations are used to present a new, alternative model of the galaxy A0035-324 (the "Cartwheel"), which is the most striking example of the relatively small class of ring galaxies. The model is based on the gravitational Jeans-type instability of both axisymmetric (radial) and nonaxisymmetric (spiral) small-amplitude gravity perturbations (e.g., those produced by spontaneous disturbances) of a dynamically cold subsystem (identified as the gaseous component) of an isolated disk galaxy. The simplified model of a galaxy is used in which stars (and a dark matter, if it exists at all) do not participate in the disk collective oscillations and just form a background charge. In the theory presented here, a case for both purely radial solutions and purely spiral solutions to the equations of motion of an infinitesimally thin gaseous disk is made, which is associated with both a radial density wave and a dominant spiral density wave which propagate outwards creating a rough ring and a number of spiral arms. Through three-dimensional numerical simulation of a collisionless set of many particles, I associate these gravitationally unstable axisymmetric waves and nonaxisymmetric waves with growing clumps of matter which take on the appearance of a ring and spokes of mass blobs.

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AHubble Space TelescopeStudy of Star Formation in the Inner Resonance Ring of NGC 3081

Cited by 30 publications

References 56 publications

Secular evolution in disk galaxies

Secular evolution in disk galaxies

The Classification of Galaxies

Origin of the Cartwheel Galaxy: Disk Instability?

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