Encounter‐triggered Disk Mass Loss in the Orion Nebula Cluster

Olczak, C.; Pfalzner, Susanne; Spurzem, Rainer

doi:10.1086/501044

Cited by 72 publications

(153 citation statements)

References 32 publications

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“…(12) will be evaluated for three different stellar masses, representing stellar mass groups of low-, intermediate-and high-mass stars. Appropriate typical interaction radii have been taken from Table 3 of Olczak et al (2006). The set of masses m , radii r enc , and "encounter escape speeds" v enc resulting from Eq.…”

Section: Comparison Of Numerical Results and Analytical Estimatesmentioning

confidence: 99%

“…minimum 3 % disc-mass loss, cf. Olczak et al 2006), the light grey those that removed at least 50 % of the discmass, while the dark grey stands for the most destructive encounters that caused a disc-mass loss of at least 90 %. The two plots show the distributions for the model D4.…”

Section: Validation Of the Numerical Methodsmentioning

confidence: 99%

“…But it is also interesting to note that even in a cluster 4 times less dense than the ONC (model D0), still 10-15 % of the stars could lose their surrounding discs due to gravitational interactions with cluster members. However, one has to treat these numbers with care due to the -partiallysignificant uncertainties that go into the calculations (see Olczak et al 2006). Nonetheless, what is more important here -and relies only on the relative quantities -is the fact that the distributions in Fig.…”

Section: Encounter Dynamicsmentioning

confidence: 99%

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Stellar interactions in dense and sparse star clusters

Olczak

Pfalzner

Eckart

2010

A&A

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Context. Stellar encounters potentially affect the evolution of the protoplanetary discs in the Orion Nebula Cluster (ONC). However, the role of encounters in other cluster environments is less known. Aims. We investigate the effect of the encounter-induced disc-mass loss in different cluster environments. Methods. Starting from an ONC-like cluster we vary the cluster size and density to determine the correlation of collision time scale and disc-mass loss. We use the nbody6++ code to model the dynamics of these clusters and analyze the disc-mass loss due to encounters. Results. We find that the encounter rate depends strongly on the cluster density but remains rather unaffected by the size of the stellar population. This dependency translates directly into the effect on the encounter-induced disc-mass loss. The essential outcome of the simulations are: i) Even in clusters four times sparser than the ONC the effect of encounters is still apparent. ii) The density of the ONC itself marks a threshold: in less dense and less massive clusters it is the massive stars that dominate the encounter-induced disc-mass loss whereas in denser and more massive clusters the low-mass stars play the major role for the disc mass removal. Conclusions. It seems that in the central regions of young dense star clusters -the common sites of star formation -stellar encounters do affect the evolution of the protoplanetary discs. With higher cluster density low-mass stars become more heavily involved in this process. This finding allows for the extrapolation towards extreme stellar systems: in case of the Arches cluster one would expect stellar encounters to destroy the discs of most of the low-and high-mass stars in several hundred thousand years, whereas intermediate mass stars are able to retain to some extant their discs even under these harsh environmental conditions.

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Section: Comparison Of Numerical Results and Analytical Estimatesmentioning

confidence: 99%

Section: Validation Of the Numerical Methodsmentioning

confidence: 99%

Section: Encounter Dynamicsmentioning

confidence: 99%

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Stellar interactions in dense and sparse star clusters

Olczak

Pfalzner

Eckart

2010

A&A

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“…Johnstone et al 1998;Störzer & Hollenbach 1999;Scally & Clarke 2002;Matsuyama et al 2003;Johnstone et al 2004;Adams et al 2006;Alexander et al 2006;Ercolano et al 2008;Gorti & Hollenbach 2009;Drake et al 2009) and stellar fly-bys or gravitational stripping (see e.g. Clarke & Pringle 1993;Scally & Clarke 2002;Pfalzner 2004;Adams et al 2006;Olczak et al 2006Olczak et al , 2010Pfalzner & Olczak 2007;Craig & Krumholz 2013;Rosotti et al 2014). From observations, the sizes of protoplanetary discs are usually determined by fitting the spectral energy distributions (SEDs) to disc models using a truncated power-law (Andrews & Williams 2007).…”

Section: Introductionmentioning

confidence: 99%

“…They derived the disc size assuming that all material outside the Lagrangian point between the two stars is stripped from the disc. Furthermore, they suggested to convert the formula for disc-mass loss for parabolic, coplanar encounters reported by Olczak et al (2006) directly into an upper limit for disc truncation, assuming a mass-density distribution within the disc of Σ = r −1 . The few previous studies that considered disc sizes in stellar cluster environments (Adams et al 2006;Malmberg et al 2011;Pfalzner 2013) generalised, for lack of a universal description of disc sizes, the results obtained for equal-mass encounter by Kobayashi & Ida (2001) to non-equal mass encounters.…”

Section: Introductionmentioning

confidence: 99%

Strong effect of the cluster environment on the size of protoplanetary discs?

Vincke

Breslau

Pfalzner

2015

A&A

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Context. Most stars are born in clusters, thus the protoplanetary discs surrounding the newly formed stars might be influenced by this environment. Isolated star-disc encounters have previously been studied, and it was shown that very close encounters are necessary to completely destroy discs. However, relatively distant encounters are still able to change the disc size considerably. Aims. We quantify the importance of disc-size reduction that is due to stellar encounters in an entire stellar population. Methods. We modelled young, massive clusters of different densities using the code Nbody6 to determine the statistics of stellar encounter parameters. In a second step, we used these parameters to investigate the effect of the environments on the disc size. For this purpose, we performed a numerical experiment with an artificial initial disc size of 10 5 AU. Results. We quantify to which degree the disc size is more sensitive to the cluster environment than to the disc mass or frequency. We show that in all investigated clusters a large portion of discs is significantly reduced in size. After 5 Myr, the fraction of discs smaller than 1000 AU in ONC-like clusters with an average number density of ρ cluster ∼ 60 pc −3 , the fraction of discs smaller than 1000 AU is 65%, while discs smaller than 100 AU make up 15%. These fractions increase to 84% and 39% for discs in denser clusters like IC 348 (ρ cluster ∼ 500 pc −3 ). Even in clusters with a density four times lower than in the ONC (ρ cluster ∼ 15 pc −3 ), about 43% of all discs are reduced to sizes below 1000 AU and roughly 9% to sizes below 100 AU. Conclusions. For any disc in the ONC that initially was larger than 1000 AU, the probability to be truncated to smaller disc sizes as a result of stellar encounters is quite high. Thus, among other effects, encounters are important in shaping discs and potentially forming planetary systems in stellar clusters.

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Concluding Issues

Clarke

2015

Dynamics of Young Star Clusters and Associations

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Encounter‐triggered Disk Mass Loss in the Orion Nebula Cluster

Cited by 72 publications

References 32 publications

Stellar interactions in dense and sparse star clusters

Stellar interactions in dense and sparse star clusters

Strong effect of the cluster environment on the size of protoplanetary discs?

Concluding Issues

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