On the structure of tidal tails

Küpper, Andreas H. W.; Macleod, Andrew; Heggie, Douglas C.

doi:10.1002/asna.200811069

Cited by 5 publications

(5 citation statements)

References 21 publications

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“…On the one hand, streams intrinsically host variations in their densities, as shown by early numerical experiments by Combes et al (1999). Küpper et al (2008) explained that the motions of stars along streams lead to orbital crowding at the epicycles (i.e. a slowing down of the stars at a fixed position, see also Capuzzo Dolcetta et al 2005).…”

Section: Stellar Streamsmentioning

confidence: 99%

Star clusters in evolving galaxies

Renaud

2018

New Astronomy Reviews

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Their ubiquity and extreme densities make star clusters probes of prime importance of galaxy evolution. Old globular clusters keep imprints of the physical conditions of their assembly in the early Universe, and younger stellar objects, observationally resolved, tell us about the mechanisms at stake in their formation. Yet, we still do not understand the diversity involved: why is star cluster formation limited to 10 5 M objects in the Milky Way, while some dwarf galaxies like NGC 1705 are able to produce clusters 10 times more massive? Why do dwarfs generally host a higher specific frequency of clusters than larger galaxies? How to connect the present-day, often resolved, stellar systems to the formation of globular clusters at high redshift? And how do these links depend on the galactic and cosmological environments of these clusters? In this review, I present recent advances on star cluster formation and evolution, in galactic and cosmological context. The emphasis is put on the theory, formation scenarios and the effects of the environment on the evolution of the global properties of clusters. A few open questions are identified.

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Section: Stellar Streamsmentioning

confidence: 99%

Star clusters in evolving galaxies

Renaud

2018

New Astronomy Reviews

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“…The data show a linear trend which almost follow same slope. For the nbody6 results as shown in Fig.2 (6) which shows the speed of evolution for a GC only due to two body relaxation mechanism in lack of existence of external tidal field. However a GC without exposure to external tidal field evolves and loses some of its stars due to two-body relaxation mechanism, but N-body simulations [16] have shown that for isolated clusters this process is inefficient in dissolving star clusters since even low-mass clusters would need more than whole life time of the universe to completely evaporate and dissolve.…”

Section: Simulation Results and Disscusionmentioning

confidence: 92%

“…On the observational side, the evidence for differences in the stellar mass-functions of globular clusters [1,2], which are believed to be at least partly the result of their dynamical evolution, and the discovery of extratidal stars surrounding globular clusters so-called tidal tails [3,4] are strong indications for the ongoing dynamical evolution and dissolution of globular clusters. The tidal tails of globular clusters have been simulated and virtualized by some authors [5][6][7]. According to the relatively low distance among the stars in globular clusters and also definition of the relaxation time, they are classified as collisional systems.…”

Section: Introductionmentioning

confidence: 99%

The effect of external tidal field on life-time of star clusters in collisional and collision-less codes

Haghi

2015

2015 International Young Scientists Forum on Applied Physics (YSF)

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The results of several performed N-body simulations using a collisionless N-body code named NMODY are reported here which aim at studying the evolution and life-time of star clusters under influence of an external tidal field. The code does not include stellar evolution, two body relaxation, and external tidal field as well. Having added the external tidal field to the code, we simulated our model clusters which are moving in circular orbits, in different galactocentric distances with various half-mass radius and initial mass around the Galaxy. Thereafter the results are compared with those of claimed by collisional code Nbody6. As the relaxation plays a main role in evolution of collisional systems, the main focus is to study how using an either collisional or collisionless code, changes the life-time of clusters. Finally the obtained relations between life-time of globular clusters with their initial half-mass radius are presented which numerically and virtually examine the strength of evolutionary mechanisms of globular clusters.

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“…It is well known that when stars escape from star clusters through the Lagrangian points form complicated structures known as tidal tails or tidal arms (e.g., [17,38,61,67,68]).…”

Section: Formation Of Spiral Armsmentioning

confidence: 99%

Escape dynamics and fractal basin boundaries in Seyfert galaxies

Zotos

2015

Nonlinear Dyn

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The escape dynamics in a simple analytical gravitational model which describes the motion of stars in a Seyfert galaxy is investigated in detail. We conduct a thorough numerical analysis distinguishing between regular and chaotic orbits as well as between trapped and escaping orbits, considering only unbounded motion for several energy levels. In order to distinguish safely and with certainty between ordered and chaotic motion, we apply the Smaller ALingment Index (SALI) method. It is of particular interest to locate the escape basins through the openings around the collinear Lagrangian points L 1 and L 2 and relate them with the corresponding spatial distribution of the escape times of the orbits. Our exploration takes place both in the physical (x, y) and in the phase (x,ẋ) space in order to elucidate the escape process as well as the overall orbital properties of the galactic system. Our numerical analysis reveals the strong dependence of the properties of the considered escape basins with the total orbital energy, with a remarkable presence of fractal basin boundaries along all the escape regimes. It was also observed, that for energy levels close to the critical escape energy the escape rates of orbits are large, while for much higher values of energy most of the orbits have low escape periods or they escape immediately to infinity. We also present evidence obtained through numerical simulations that our model can describe the formation and the evolution of the observed spiral structure in Seyfert galaxies. We hope our outcomes to be useful for a further understanding of the escape mechanism in galaxies with active nuclei.

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On the structure of tidal tails

Cited by 5 publications

References 21 publications

Star clusters in evolving galaxies

Star clusters in evolving galaxies

The effect of external tidal field on life-time of star clusters in collisional and collision-less codes

Escape dynamics and fractal basin boundaries in Seyfert galaxies

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