On the Problem of Distribution in Globular Star Clusters: (Plate 8.)

Plummer, H. C.

doi:10.1093/mnras/71.5.460

Cited by 1,584 publications

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“…In Fig. 2 we show the results for different shock strengths, for the isochrone model (Hénon 1959;Hénon 1960), the Jaffe model (Jaffe 1983) and the Plummer model (Plummer 1911), all truncated at 100r h . Elson, Fall & Freeman (1987) and Mackey & Gilmore (2003) find in a sample of young clusters in the Large Magellanic Cloud that most clusters have luminosity profiles with logarithmic slopes between −2.5 and −3 in the outer regions, corresponding to −3.5 and −4 after de-projecting under the assumption of spherical symmetry.…”

Section: Density Evolutionmentioning

confidence: 99%

If it does not kill them, it makes them stronger: collisional evolution of star clusters with tidal shocks

Gieles

Renaud

2016

Monthly Notices of the Royal Astronomical Society: Letters

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The radii of young ( 100 Myr) star clusters correlate only weakly with their masses. This shallow relation has been used to argue that impulsive tidal perturbations, or 'shocks', by passing giant molecular clouds (GMCs) preferentially disrupt low-mass clusters. We show that this mass-radius relation is in fact the result of the combined effect of two-body relaxation and repeated tidal shocks. Clusters in a broad range of environments including those like the solar neighbourhood evolve towards a typical radius of a few parsecs, as observed, independent of the initial radius. This equilibrium mass-radius relation is the result of a competition between expansion by relaxation and shrinking due to shocks. Interactions with GMCs are more disruptive for low-mass clusters, which helps to evolve the globular cluster mass function (GCMF). However, the properties of the interstellar medium in high-redshift galaxies required to establish a universal GCMF shape are more extreme than previously derived, challenging the idea that all GCs formed with the same power-law mass function.

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Section: Density Evolutionmentioning

confidence: 99%

If it does not kill them, it makes them stronger: collisional evolution of star clusters with tidal shocks

Gieles

Renaud

2016

Monthly Notices of the Royal Astronomical Society: Letters

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“…Stellar masses are drawn from a Kroupa, Tout, & Gilmore (1993) initial mass function between 0.1M⊙ and 30M⊙, with each star assigned a metallicity of Z = 0.001. The distribution of stellar positions and velocities follow a Plummer density profile with a cutoff at 10rm (Plummer 1911;Aarseth et al 1974). The initial half mass radius of each model is set to 6 pc, which ensures that all models exhibit bound stars at or beyond rt and can be considered tidally filling.…”

Section: The Modelsmentioning

confidence: 99%

The effects of orbital inclination on the scale size and evolution of tidally filling star clusters

Webb

Sills

Harris

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We have performed N -body simulations of tidally filling star clusters with a range of orbits in a Milky Way-like potential to study the effects of orbital inclination and eccentricity on their structure and evolution. At small galactocentric distances R gc , a non-zero inclination results in increased mass loss rates. Tidal heating and disk shocking, the latter sometimes consisting of two shocking events as the cluster moves towards and away from the disk, help remove stars from the cluster. Clusters with inclined orbits at large R gc have decreased mass loss rates than the non-inclined case, since the strength the disk potential decreases with R gc . Clusters with inclined and eccentric orbits experience increased tidal heating due to a constantly changing potential, weaker disk shocks since passages occur at higher R gc , and an additional tidal shock at perigalacticon. The effects of orbital inclination decrease with orbital eccentricity, as a highly eccentric cluster spends the majority of its lifetime at a large R gc . The limiting radii of clusters with inclined orbits are best represented by the r t of the cluster when at its maximum height above the disk, where the cluster spends the majority of its lifetime and the rate of change in r t is a minimum. Conversely, the effective radius is independent of inclination in all cases.

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“…We model this progenitor as a Plummer sphere (Plummer 1911) with different Plummer radii R pl and initial masses M pl . A Plummer sphere is a widely used representation to model a young stellar cluster (e.g., Boily & Kroupa 2003).…”

Section: Methods and Setupmentioning

confidence: 99%

Could Segue 1 be a destroyed star cluster? – a dynamical perspective

Domínguez

Fellhauer

Blaña

et al. 2016

Mon. Not. R. Astron. Soc.

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We attempt to find a progenitor for the ultra-faint object Segue 1 under the assumption that it formed as a dark matter free star cluster in the past. We look for orbits, using the elongation of Segue 1 on the sky as a tracer of its path. Those orbits are followed backwards in time to find the starting points of our N-body simulations. The successful orbit, with which we can reproduce Segue 1 has a proper motion of µ α = −0.19 mas yr −1 and µ δ = −1.9 mas yr −1 , placing Segue 1 near its apo-galacticon today. Our best fitting model has an initial mass of 6224 M ⊙ and an initial scale-length of 5.75 pc.

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On the Problem of Distribution in Globular Star Clusters: (Plate 8.)

Cited by 1,584 publications

References 0 publications

If it does not kill them, it makes them stronger: collisional evolution of star clusters with tidal shocks

If it does not kill them, it makes them stronger: collisional evolution of star clusters with tidal shocks

The effects of orbital inclination on the scale size and evolution of tidally filling star clusters

Could Segue 1 be a destroyed star cluster? – a dynamical perspective

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