Formation of Double Galaxies by Tidal Capture

Sastry, K. S.; Potdar, A.; Alladin, S. M.

doi:10.1007/978-94-010-1818-0_17

Cited by 11 publications

(4 citation statements)

References 5 publications

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“…However the disruptive effect of encounters with interstellar clouds is less important than that of disk shocking (Chernoff et al 1986). Bulge shocking has been considered by Alladin et al (1976), Aguilar & White (1985), Spitzer (1987), Weinberg (1994b), and Charlton & Laguna (1995).…”

Section: Tidal Truncationmentioning

confidence: 99%

Internal Dynamics of Globular Clusters

Meylan¹

2000

The Chaotic Universe

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Galactic globular clusters are ancient building blocks of our Galaxy. They represent a very interesting family of stellar systems in which some fundamental dynamical processes have been taking place for more than 10 Gyr, but on time scales shorter than the age of the universe. In contrast with galaxies, these star clusters represent unique laboratories for learning about two-body relaxation, mass segregation from equipartition of energy, stellar collisions, stellar mergers, core collapse, and tidal disruption. This review briefly summarizes some of the tremendous developments that have taken place during the last two decades. It ends with some recent results on tidal tails around galactic globular clusters and on a very massive globular cluster in M31.

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Section: Tidal Truncationmentioning

confidence: 99%

Internal Dynamics of Globular Clusters

Meylan¹

2000

The Chaotic Universe

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“…The speciÐc conditions under which galaxy mergers occur are still somewhat uncertain. The analytical work carried out under an impulsive approximation (see, e.g., Alladin 1965 ;Alladin, Potdar, & Sastry 1975 ;White 1982 and references therein) has indicated that tidal interactions will dissipate sufficient orbital energy to e †ect capture if the original encounter velocity between the two galaxies is slightly hyperbolic or less. More speciÐcally, the energy dissipation from tidal interaction scales as…”

Section: Appendixmentioning

confidence: 99%

On the Origins of Starburst and Poststarburst Galaxies in Nearby Clusters

Caldwell

Rose

Dendy

1999

The Astronomical Journal

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Hubble Space T elescope (HST ) Wide Field Planetary Camera 2 images in B (F450W) and I (F814W) have been obtained for three starburst (SB) and two poststarburst (PSB) galaxies in the Coma Cluster and for three such galaxies in the cluster DC 048[52. V (F555W) and I images for an additional PSB galaxy in Coma have been extracted from the HST archive. Six of these galaxies were previously classiÐed as E/S0 on the basis of ground-based images, two as Sa, and the other as an irregular.The HST images reveal these SB/PSB galaxies to be heterogeneous in morphology. Nevertheless, a common theme is that many of them, especially the SB galaxies, tend to have centralized spiral structure that appears simply as a bright "" bulge ÏÏ on ground-based images. In addition, while some PSB galaxies exhibit distinct spiral structure, on the whole they have smoother morphologies than the SB galaxies. The morphologies and luminosity proÐles are generally consistent with substantial starbursts, in the form of centralized spiral structure (the SB galaxies), that fade into smoother morphologies (the PSB galaxies), with lingering spectroscopic evidence for past central starbursts. An important point is that the PSB galaxies retain disks ; i.e., they have not evolved into spheroidal systems.While the morphologies revealed in the HST images are heterogeneous, and thus may not Ðt well into a single picture, we see evidence in several cases that the morphologies and centralized star formation have been driven by external tidal perturbations. We discuss several physical mechanisms for inducing star formation in cluster galaxies with a view toward explaining the particular morphologies seen in the HST images.

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“…Also, Oort (1970) has shown via simple models that one should in general expect ambient matter to continue to fall into a galaxy for a long time after it has formed. Tidal interactions between neighboring young galaxies may also continue to exert important effects on their structure and dynamics, and galaxies may even collide inelastically and merge to form larger systems (Toomre and Toomre, 1972;Alladin et al, 1975).…”

Section: Simple Collapse Vs Clustering or Accretionmentioning

confidence: 99%

The Collapse and Formation of Galaxies

Larson

1975

Symp. - Int. Astron. Union

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The ultimate aim of studies of the dynamics of stellar systems is to gain an understanding of why they have the structures that are observed, how they might have formed, and how they might evolve with time. In the case of galaxies, unlike smaller astronomical systems such as stars and star clusters, the problem of understanding their present structure is inseparable from the problem of understanding their formation since, as has long been clear, the two-body relaxation time in galaxies is much longer than the age of the universe, so that properties such as the radial density distribution and the flattening of elliptical galaxies cannot have changed significantly since they were formed. Other features of galaxies, such as the presence of spiral patterns or nuclear activity, may be of a more transitory nature and not closely related to the formation process, but such phenomena probably involve mainly the gas component of galaxies and may be regarded as perturbations on the underlying stellar system, whose basic structure must still be understood in terms of the formation process.

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Formation of Double Galaxies by Tidal Capture

Cited by 11 publications

References 5 publications

Internal Dynamics of Globular Clusters

Internal Dynamics of Globular Clusters

On the Origins of Starburst and Poststarburst Galaxies in Nearby Clusters

The Collapse and Formation of Galaxies

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