On the interpretation of ring galaxies : the binary ring system II Hz4.

Lynds, Roger; Toomre, Alar

doi:10.1086/154730

Cited by 240 publications

(200 citation statements)

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“…The density wave created by the collision empties the central region of the disk and forms a ring in radial expansion (Lynds & Toomre 1976, see also Appleton & Struck-Marcell 1996 for an observational and theoretical review).…”

Section: Rings Ripples Shells and Warpsmentioning

confidence: 99%

Tides in Colliding Galaxies

Duc

Renaud

2013

Lecture Notes in Physics

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Long tails and streams of stars are the most noticeable upshots of galaxy collisions. Their origin as gravitational, tidal, disturbances has however been recognized only less than fifty years ago and more than ten years after their first observations. This Review describes how the idea of galactic tides emerged, in particular thanks to the advances in numerical simulations, from the first ones that included tens of particles to the most sophisticated ones with tens of millions of them and state-of-the-art hydrodynamical prescriptions. Theoretical aspects pertaining to the formation of tidal tails are then presented. The third part of the review turns to observations and underlines the need for collecting deep multi-wavelength data to tackle the variety of physical processes exhibited by collisional debris. Tidal tails are not just stellar structures, but turn out to contain all the components usually found in galactic disks, in particular atomic / molecular gas and dust. They host star-forming complexes and are able to form star-clusters or even second-generation dwarf galaxies. The final part of the review discusses what tidal tails can tell us (or not) about the structure and content of present-day galaxies, including their dark components, and explains how tidal tails may be used to probe the past evolution of galaxies and their mass assembly history. On-going deep wide-field surveys disclose many new lowsurface brightness structures in the nearby Universe, offering great opportunities for attempting galactic archeology with tidal tails.

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Section: Rings Ripples Shells and Warpsmentioning

confidence: 99%

Tides in Colliding Galaxies

Duc

Renaud

2013

Lecture Notes in Physics

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“…The basic observational properties of a sample of RGs were determined in the 70s by Theys & Spiegel (1976 and their earliest numerical simulation regarding their origin were carried out by Lynds & Toomre (1976). Multiple-band observations were performed by Appleton & Struck-Marcell (1997, and references therein).…”

Section: Introductionmentioning

confidence: 99%

The ring galaxy HRG 54 103: a first study

Faúndez-Abans

Fernandes

Oliveira-Abans

et al. 2009

A&A

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Aims. We report the first study of the peculiar ring galaxy HRG 54103 which was previously classified as a Saturn-like type galaxy. Methods. The study is based on low resolution spectroscopy and photometric observations in the optical band to highlight the characteristics of this almost isolated galaxy. The colour distribution of HRG 54103 was examined through direct CCD BVRI Kron-Cousins system imagery. Color-color diagrams of the bulge and ring are displayed and further compared with the star-forming ring galaxy HRG 2302.Results. The results of image enhancement of the morphological structure of this galaxy are discussed. The nuclear emission-line spectrum resembles that of a Seyfert2/LINER object, with z = 0.022 and heliocentric V = 6483 ± 18 km s −1 , in agreement with the literature. The nuclear, bulge and ring section radial velocities along the ring major axis show a peculiar distribution, which together and the disk-ring asymmetry suggest a possible merger event in the recent past of this object, which could also have caused its formation.

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“…Strong interactions also form ring galaxies (Theys & Spiegel 1976;Lynds & Toomre 1976), polar ring galaxies (e.g., Cox & Sparke 2004), disk warps, tidal tails, and so on (Toomre & Toomre 1972). Secular interactions include accretion in the form of residual hierarchical build-up from outside the galaxy, continuous accretion of dwarfs (e.g., Lewis et al 2004), galaxy harassment (e.g., Moore et al 1996), accretion of gas (e.g., , globular cluster accretion from dwarfs (e.g., Bellazzini, Ibata, & Ferraro 2004), halo streams (e.g., Ferguson et al 2005), and so on.…”

Section: Summary Of Evolutionary Effects Over a Hubble Timementioning

confidence: 99%

Bars, Spiral Structure, and Secular Evolution in Disk Galaxies

Elmegreen¹

Island Universes

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Simulations and observations of galactic bars suggest they do not commonly evolve into bulges, although it is possible that the earliest bars formed bulges long ago, when galaxies were smaller, denser, and had more gas. The most highly evolved of today's bars may become lenses over a Hubble time. Most galaxies in the early Universe are extremely clumpy, with ∼ 10 8 − 10 9 M⊙ blue clumps that resemble in color and magnitude the isolated field objects nearby. The presence of blue and irregular bars at high redshift suggests that some bars formed primarily in the gas phase accompanied by giant starbursts, rather than in pure stellar disks like most models. Secular and non-secular processes that cause galaxies to evolve are summarized.

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On the interpretation of ring galaxies : the binary ring system II Hz4.

Cited by 240 publications

References 0 publications

Tides in Colliding Galaxies

Tides in Colliding Galaxies

The ring galaxy HRG 54 103: a first study

Bars, Spiral Structure, and Secular Evolution in Disk Galaxies

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