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

Vincke, Kirsten; Breslau, Andreas; Pfalzner, Susanne

doi:10.1051/0004-6361/201425552

Cited by 83 publications

(89 citation statements)

References 67 publications

(133 reference statements)

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“…In particular, the disk size might be strongly influenced by the presence of other cluster members (Vincke et al 2015). Most of the investigations so far have considered the effect of parabolic, coplanar encounters on the disk size.…”

Section: Discussionmentioning

confidence: 99%

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Effects of inclined star-disk encounter on protoplanetary disk size

Bhandare

Breslau

Pfalzner

2016

A&A

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Most, if not all, young stars are initially surrounded by protoplanetary disks. Owing to the preferential formation of stars in stellar clusters, the protoplanetary disks around these stars may potentially be affected by the cluster environment. Various works have investigated the influence of stellar fly-bys on disks, although many of them consider only the effects due to parabolic, coplanar encounters often for equal-mass stars, which is only a very special case. We perform numerical simulations to study the fate of protoplanetary disks after the impact of parabolic star-disk encounter for the less investigated case of inclined up to coplanar, retrograde encounters, which is a much more common case. Here, we concentrate on the disk size after such encounters because this limits the size of the potentially forming planetary systems. In addition, with the possibilities that ALMA offers, now a direct comparison to observations is possible. Covering a wide range of periastron distances and mass ratios between the mass of the perturber and central star, we find that despite the prograde, coplanar encounters having the strongest effect on the disk size, inclined and even the least destructive retrograde encounters mostly also have a considerable effect, especially for close periastron passages. Interestingly, we find a nearly linear dependence of the disk size on the orbital inclination for the prograde encounters, but not for the retrograde case. We also determine the final orbital parameters of the particles in the disk such as eccentricities, inclinations, and semi-major axes. Using this information the presented study can be used to describe the fate of disks and also that of planetary systems after inclined encounters.

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Section: Discussionmentioning

confidence: 99%

“…This is important, for example, if one post-processes cluster simulations to determine the average disk size change due to encounters (Vincke et al 2015). We found a dependence of the disk size on the mass ratio and periastron distance which is represented by the fit formula of the form…”

Section: Dependence On Mass Ratio and Periastron Distancementioning

confidence: 92%

Effects of inclined star-disk encounter on protoplanetary disk size

Bhandare

Breslau

Pfalzner

2016

A&A

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“…Survival of disks in general, however, might not be as short as the age determined in these studies. Indeed, in clusters, the rich stellar environment may enhance the disk dispersal and lead to shorter lifetime estimates than for isolated stars (Pfalzner et al 2014;Vincke et al 2015). Pfalzner et al (2014) evaluate that at least 30%, and possibly as much as 50%, of the disks are living for more than 10 Myr.…”

Section: A Possible Diagram Of Evolutionmentioning

confidence: 99%

The hybrid disks: a search and study to better understand evolution of disks

Péricaud

Folco

Dutrey

et al. 2017

A&A

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Context. The increased sensitivity of millimeter-wave facilities now makes possible the detection of low amounts of gas in debris disks. Some of the gas-rich debris disks harbor peculiar properties, with possible pristine gas and secondary generated dust. The origin of the gas in these hybrid disks is strongly debated and the current sample is too sparse to understand this phenomenon. Aims. More detections are necessary to increase the statistics on this population. Lying at the final stages of evolution of protoplanetary disks and at the beginning of the debris disk phase, these objects could provide new insight into the processes involved in the making of planetary systems. Methods. We carried out a deep survey of the CO J=2→1 and CO J=3→2 lines with the APEX and IRAM radiotelescopes in young debris disks selected according to hybrid disk properties. The survey is complemented with a bibliographic study of the ratio between the emission of the gas and the continuum (S CO /F cont ) in CTTS, Herbig Ae, WTTS, hybrid, and debris disks. Results. Our sub-mm survey comprises 25 stars, including 17 new targets, and we increase the sensitivity limit by a factor 2 on eight sources compared to similar published studies. We report a 4 σ tentative detection of a double-peaked CO J=2→1 line around HD 23642; an eclipsing binary located in the Pleiades. We also reveal a correlation between the emission of the CO gas and the dust continuum from CTTS, Herbig Ae and few debris disks. The observed trend of the gas to dust flux ratio suggests a concurrent dissipation of the dust and gas components. Hybrid disks systematically lie above this trend, suggesting that these systems may witness a transient phase, when the dust has evolved more rapidly than the gas, with a flux ratio S CO /F cont enhanced by a factor of between 10 and 100 compared to standard (proto-)planetary disks.

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“…However, none of these studies considered the gas content as such or the effect that the gas expulsion process has on the cluster dynamics. Here we want to concentrate instead on the disksize, because (a) it is the most sensitive indicator for the cluster influence (Rosotti et al 2014;Vincke et al 2015), (b) with the advent of ALMA, a direct comparison with observations is possible, and (c) it gives limits on the sizes of the potentially forming planetary systems that can be compared to exoplanetary systems.…”

Section: Introductionmentioning

confidence: 99%

Cluster Dynamics Largely Shapes Protoplanetary Disk sizes

Vincke

Pfalzner

2016

ApJ

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104

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

Cited by 83 publications

References 67 publications

Effects of inclined star-disk encounter on protoplanetary disk size

Effects of inclined star-disk encounter on protoplanetary disk size

The hybrid disks: a search and study to better understand evolution of disks

Cluster Dynamics Largely Shapes Protoplanetary Disk sizes

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