The Evolution of Protoplanetary Disks in the Arches Cluster

Olczak, C.; Kaczmarek, Thomas; Harfst, Stefan; Pfalzner, Susanne; Zwart, Simon Portegies

doi:10.1088/0004-637x/756/2/123

Cited by 39 publications

(46 citation statements)

References 81 publications

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“…The overall disk fraction for the B stars in the Arches cluster is 6%, much lower than what would expect from the disk fraction age relation (Haisch et al 2001). They explain the decrease in disk fraction toward the center by either UV radiation destruction, winds, or the tidal destruction mechanism of Olczak et al (2012) that has the important characteristic, in the context of this work, of destroying the disk without destroying the dust.…”

Section: Discussionmentioning

confidence: 70%

The central density of R136 in 30 Doradus

Selman

Melnick

2013

A&A

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The central density, ρ 0 , of a stellar cluster is an important physical parameter for determining its evolutionary and dynamical state. How much mass segregation there is or whether the cluster has undergone core collapse both depend on ρ 0 . We reanalyze the results of a previous paper that gives the mass density profile of R136 and combine them with both a conservative upper limit for the core parameter and a more uncertain recent measurement. We thus place a lower limit on ρ 0 under reasonable and defensible assumptions about the IMF, finding ρ 0 ≥ 1.5 × 10 4 M /pc 3 for the conservative assumption a < 0.4 pc for the cluster core parameter. If we use the lower, but more uncertain value a = 0.025 pc, the central density estimate becomes greater than 10 7 M /pc 3 . A mechanism based on the destruction of a large number of circumstellar disks is posited to explain the hitherto unexplained increase in reddening presented in that same work.

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Section: Discussionmentioning

confidence: 70%

The central density of R136 in 30 Doradus

Selman

Melnick

2013

A&A

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“…For the denser cluster models (especially E52), a detailed study of the influence of hyperbolic fly-bys on disksizes would be favorable. Previous studies suggest that their influence on the disks (in these cases, the diskmass and angular momentum) is much smaller than the one of parabolic encounters (for detailed discussions, see, e.g., Pfalzner et al 2005c;Olczak et al 2010Olczak et al , 2012. Therefore, the disksizes presented here might be lower limits.…”

Section: Appendix Fly-by Velocity and Eccentricitymentioning

confidence: 63%

Cluster Dynamics Largely Shapes Protoplanetary Disk sizes

Vincke

Pfalzner

2016

ApJ

103

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To what degree the cluster environment influences the sizes of protoplanetary disks surrounding young stars is still an open question. This is particularly true for the short-lived clusters typical for the solar neighborhood, in which the stellar density and therefore the influence of the cluster environment change considerably over the first 10 Myr. In previous studies,the effect of the gas on the cluster dynamics has oftenbeen neglected;this is remedied here. Using the code NBody6++,we study the stellar dynamics in different developmental phases-embedded, expulsion, and expansion-including the gas, and quantify the effect of fly-bys on the disksize. We concentrate on massive clusters (M cl 10 3 -6 * 10 4 M Sun ), which are representative for clusters like the Orion Nebula Cluster (ONC) or NGC 6611. We find that not only the stellar density but also the duration of the embedded phase matters. The densest clusters react fastest to the gas expulsion and drop quickly in density, here 98% of relevant encounters happen before gas expulsion. By contrast, disks in sparser clusters are initially less affected, but because these clusters expand moreslowly,13% of disks are truncated after gas expulsion. For ONC-like clusters, we find that disks larger than 500 au are usuallyaffected by the environment, which corresponds to the observation that 200 ausized disks are common. For NGC 6611-like clusters, disksizes are cut-down on average to roughly 100 au. A testable hypothesis would be that the disks in the center of NGC 6611 should be on average ≈20 au and therefore considerably smaller than those in the ONC.

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“…This change was already noticed in the context of the influence of encounters on protoplanetary discs (Olczak et al 2010;Duke & Krumholz 2012;Olczak et al 2012;Pfalzner 2013). It was found there that parabolic encounters with low-mass stars (<0.5 M ) and the few most massive stars of the system dominate at mean cluster densities of ≈10 3 pc −3 .…”

Section: Nature Of the Encounter-induced Mass Lossmentioning

confidence: 69%

Reaction of massive clusters to gas expulsion – The cluster density dependence

Pfalzner

Kaczmarek

2013

A&A

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Context. The expulsion of the unconverted gas at the end of the star formation process potentially leads to the expansion of the just formed stellar cluster and membership loss. The degree of expansion and mass loss depends largely on the star formation efficiency and scales with the mass and size of the stellar group when stellar interactions can be neglected. Aims. We investigate the circumstances in which stellar interactions between cluster members become so important that the fraction of bound stars after gas expulsion is significantly altered. Methods. The Nbody6 code is used to simulate the cluster dynamics after gas expulsion for different star formation efficiences. Concentrating on the most massive clusters observed in the Milky Way, we test to what extent the results depend on the model, i.e. stellar mass distribution, stellar density profile etc., and the cluster parameters, such as cluster density and size. Results. We find that stellar interactions leading to ejections are responsible for up to 20% mass loss in the most compact massive clusters in the Milky Way. Therefore, ejections are the prime mass loss process in these systems. Even in the loosely bound OB associations, stellar interactions are responsible for at least ∼5% mass loss. The main reason why the importance of encounters for massive clusters has been largely overlooked is because of the often used approach of a single-mass representation instead of a realistic distribution for the stellar masses. The density dependence on the encounter-induced mass loss is shallower than expected because of the increasing importance of few-body interactions in dense clusters compared to sparse clusters where 2-body encounters dominate.

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The Evolution of Protoplanetary Disks in the Arches Cluster

Cited by 39 publications

References 81 publications

The central density of R136 in 30 Doradus

The central density of R136 in 30 Doradus

Cluster Dynamics Largely Shapes Protoplanetary Disk sizes

Reaction of massive clusters to gas expulsion – The cluster density dependence

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