The Effects of a Stellar Encounter on a Planetesimal Disk

Kobayashi, Hiroshi; Ida, Shigeru

doi:10.1006/icar.2001.6700

Cited by 104 publications

(141 citation statements)

References 59 publications

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“…Within the ensemble of N-body simulations described above, we can find the distributions of close encounters. These distributions, in conjunction with the cross sections for disruptions of planetary systems (see x 4; Adams & Laughlin 2001), binary-disk systems (Ostriker 1994;Heller 1993Heller , 1995Kobayashi & Ida 2001), and binary-star interactions (Heggie et al 1996;Rasio et al 1995), can then be used to estimate the probability of interactions as a function of system size N (and other initial conditions).…”

Section: Distribution Of Closest Approachesmentioning

confidence: 99%

Early Evolution of Stellar Groups and Clusters: Environmental Effects on Forming Planetary Systems

Adams

Proszkow

Fatuzzo

et al. 2006

ApJ

293

391

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This paper studies the dynamical evolution of young groups/clusters, with N ¼ 100 1000 members, from their embedded stage out to ages of $10 Myr. We use N-body simulations to explore how their evolution depends on the system size N and the initial conditions. Motivated by recent observations suggesting that stellar groups begin their evolution with subvirial speeds, this study compares subvirial starting states with virial starting states. Multiple realizations of equivalent cases (100 simulations per initial condition) are used to build up a robust statistical description of these systems, e.g., the probability distribution of closest approaches, the mass profiles, and the probability distribution for the radial location of cluster members. These results provide a framework from which to assess the effects of groups/clusters on the processes of star and planet formation and to study cluster evolution. The distributions of radial positions are used in conjunction with the probability distributions of the expected far-ultraviolet (FUV ) luminosities (calculated here as a function of cluster size N ) to determine the radiation exposure of circumstellar disks. The distributions of closest approaches are used in conjunction with scattering cross sections (calculated here as a function of stellar mass using $10 5 Monte Carlo scattering experiments) to determine the probability of disruption for newly formed solar systems. We use the nearby cluster NGC 1333 as a test case in this investigation. The main conclusion of this study is that clusters in this size range have only a modest effect on forming planetary systems. The interaction rates are low, so that the typical solar system experiences a single encounter with closest approach distance b $ 1000 AU. The radiation exposure is also low, with median FUV flux G 0 $ 900 (1.4 ergs s À1 cm À2 ), so that photoevaporation of circumstellar disks is only important beyond 30 AU. Given the low interaction rates and modest radiation levels, we suggest that solar system disruption is a rare event in these clusters.

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Section: Distribution Of Closest Approachesmentioning

confidence: 99%

Early Evolution of Stellar Groups and Clusters: Environmental Effects on Forming Planetary Systems

Adams

Proszkow

Fatuzzo

et al. 2006

ApJ

293

391

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“…Nevertheless, the disc size is an important parameter because it defines the physical extent of the potentially forming planetary system. The disc size after an encounter event was investigated for example by Kobayashi & Ida (2001). They found that the disc size after an equal-mass encounter is one-third of the periastron distance.…”

Section: Introductionmentioning

confidence: 99%

“…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%

“…Recently, Breslau et al (2014) showed that a generalisation of this one-third criterion postulated by Kobayashi & Ida (2001) is not advisable and that the outcome is very sensitive to the mass ratio of the two stars. They performed simulations of isolated star-disc encounters for a wide range of periastron distances and mass ratios, choosing the highest contrast in surface density to determine the disc sizes after the encounters.…”

Section: Introductionmentioning

confidence: 99%

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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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“…Stellar flybys have been invoked to explain the high eccentricity orbits of some Kuiper belt objects such as Sedna (Kenyon & Bromley 2004), the dynamics of planetary systems (Malmberg et al 2007;Spurzem et al 2009), and the structures of debris disks (Larwood 1997;Mouillet et al 1997;Kalas et al 2000;Kobayashi & Ida 2001). Impacts of stellar flybys during A&A 532, A120 (2011) the first few million years have also been studied in the context of the evolution of protoplanetary disks and planet formation (Bonnell et al 2001;Olczack et al 2009).…”

Section: Introductionmentioning

confidence: 99%

Stripping a debris disk by close stellar encounters in an open stellar cluster

Lestrade

Morey

Lassus

et al. 2011

A&A

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A debris disk is a constituent of any planetary system surrounding a main sequence star. We study whether close stellar encounters can disrupt and strip a debris disk of its planetesimals in the expanding open cluster of its birth with a decreasing star number density over 100 Myr. Such stripping would affect the dust production and hence detectability of the disk. We tabulated the fractions of planetesimals stripped off during stellar flybys of miss distances between 100 and 1000 AU and for several mass ratios of the central to passing stars. We then estimated the numbers of close stellar encounters over the lifetime of several expanding open clusters characterized by their initial star densities. We found that a standard disk, with inner and outer radii of 40 and 100 AU, suffers no loss of planetesimals over 100 Myr around a star born in a common embedded cluster with star density ≤1000 pc −3 . In contrast, we found that such a disk is severely depleted of its planetesimals around a star born in an Orion-type cluster where the star density is >20 000 pc −3 . In this environment, a disk loses >97% of its planetesimals around an M-dwarf, >63% around a solar-type star, and >42% around an A-dwarf, over 100 Myr. We roughly estimate that two-thirds of the stars may be born in such high star density clusters. This might explain in part why fewer debris disks are observed around lower mass stars.

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The Effects of a Stellar Encounter on a Planetesimal Disk

Cited by 104 publications

References 59 publications

Early Evolution of Stellar Groups and Clusters: Environmental Effects on Forming Planetary Systems

Early Evolution of Stellar Groups and Clusters: Environmental Effects on Forming Planetary Systems

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

Stripping a debris disk by close stellar encounters in an open stellar cluster

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