Models of ring galaxies. II - Extended starbursts

Struck, Curtis; Appleton, P. N.

doi:10.1086/165846

Cited by 21 publications

(11 citation statements)

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“…Secondary, inner rings, in the outskirts of nuclear region can then form from second rebounds (see Athanassoula & Bosma 1985;Appleton & Struckf.renaud@surrey.ac.uk Marcell 1996, for reviews). Gas flows onto the nuclear region and inner ring and fuels star formation there (Struck-Marcell & Appleton 1987;Struck et al 1996). Collisions with a more off-centred impact lead to less symmetric configurations and could explain why some ring systems do not show a nuclear component, which could also result from the destruction of a loosely bound nucleus during the interaction (Madore et al 2009).…”

Section: Introductionmentioning

confidence: 99%

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Morphology and enhanced star formation in a Cartwheel-like ring galaxy

Renaud

Athanassoula

Amram

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We use hydrodynamical simulations of a Cartwheel-like ring galaxy, modelled as a nearly head-on collision of a small companion with a larger disc galaxy, to probe the evolution of the gaseous structures and flows, and to explore the physical conditions setting the star formation activity. Star formation is first quenched by tides as the companion approaches, before being enhanced shortly after the collision. The ring ploughs the disc material as it radially extends, and almost simultaneously depletes its stellar and gaseous reservoir into the central region, through the spokes, and finally dissolve 200 Myr after the collision. Most of star formation first occurs in the ring before this activity is transferred to the spokes and then the nucleus. We thus propose that the location of star formation traces the dynamical stage of ring galaxies, and could help constrain their star formation histories. The ring hosts tidal compression associated with strong turbulence. This compression yields an azimuthal asymmetry, with maxima reached in the side furthest away from the nucleus, which matches the star formation activity distribution in our models and in observed ring systems. The interaction triggers the formation of star clusters significantly more massive than before the collision, but less numerous than in more classical galaxy interactions. The peculiar geometry of Cartwheel-like objects thus yields a star (cluster) formation activity comparable to other interacting objects, but with notable second order differences in the nature of turbulence, the enhancement of the star formation rate, and the number of massive clusters formed.

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Section: Introductionmentioning

confidence: 99%

“…Such activity is rapidly evolving in time and space, as suggested by colour gradients across the structures (Marcum et al 1992;Appleton & Marston 1997) and as modelled by e.g. Struck-Marcell & Appleton (1987).…”

Section: Introductionmentioning

confidence: 99%

Morphology and enhanced star formation in a Cartwheel-like ring galaxy

Renaud

Athanassoula

Amram

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…These data have been obtained from values taken from Figure 2.4: (a)The gas density distribution for an off-center ring galaxy model (Model E) from the work of Appleton & Struck-Marcell (1987). Note that the density varies with azimuth around the ring.…”

Section: The Surface Brightness Properties Of the Ringsmentioning

confidence: 99%

A study of galaxy interactions

Charmandaris

Χαρμανδάρης²

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“…Three dozen ring galaxies were observed out to redshift z = 1.4 in these fields (Elmegreen & Elmegreen 2006b). Some ring galaxies have close companions and appear to be collisional rings such as those modeled by Struck-Marcell & Appleton (1987), while other isolated examples may be resonance rings (Buta & Combes 1996). Some galaxies look like bent chain galaxies, with apparently warped disks from interactions.…”

Section: Ring Galaxiesmentioning

confidence: 99%

Clumpy Galaxies in the Early Universe

Elmegreen

2006

Proc. IAU

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Abstract. Clumpy galaxies are prominent in the early Universe. We present morphological and photometric properties of a wide range of galaxy types and their star-forming clumps in the Hubble Ultra Deep Field. Sizes, scale lengths, and scale heights suggest that galaxies grow by a factor of 2 from z = 4 to the present, and that thick disks are present in the early Universe. The largest clumps of star formation are 10 7 -10 9 M in different galaxies, much more massive than large star-forming complexes in local galaxies. Dissolved clumps may account for both the exponential disks and the early thick disks of spirals and proto-spiral galaxies.

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Models of ring galaxies. II - Extended starbursts

Cited by 21 publications

References 0 publications

Morphology and enhanced star formation in a Cartwheel-like ring galaxy

Morphology and enhanced star formation in a Cartwheel-like ring galaxy

A study of galaxy interactions

Clumpy Galaxies in the Early Universe

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