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

Lestrade, J. F.; Morey, E.; Lassus, A.; Phou, N.

doi:10.1051/0004-6361/201014730

Cited by 34 publications

(44 citation statements)

References 55 publications

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“…Perturbation of the already formed planetary system (Malmberg et al 2007(Malmberg et al , 2011Lestrade et al 2011;Parker & Quanz 2011) by encounters did not take place, because having formed in a leaky cluster, the encounter probability for the solar system rapidly dropped as the cluster density decreased precipitately with cluster age. Even if the solar system was part of the remnant cluster after gas expulsion, the stellar density would be <1 M pc −3 , far too low to make a close encounter likely.…”

Section: Discussionmentioning

confidence: 99%

Early evolution of the birth cluster of the solar system

Pfalzner

2012

A&A

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Context. The solar system was most likely born in a star cluster containing at least 1000 stars. It is highly probable that this cluster environment influenced various properties of the solar system such as its chemical composition, size, and the orbital parameters of some of its constituting bodies. Aims. In the Milky Way, clusters with more than 2000 stars only form in two types -starburst clusters and leaky clusters -, each following a unique temporal development in the mass-radius plane. The aim is here to determine the encounter probability in the range relevant to solar system formation for starburst or leaky cluster environments as a function of cluster age. Methods. N-body methods were used to investigate the cluster dynamics and the effect of gravitational interactions between cluster members on young solar-type stars surrounded by discs. Results. Using the now available knowledge of the cluster density at a given cluster age we demonstrate that in starburst clusters the central densities over the first 5 Myr are so high (initially >10 5 M pc −3 ) that hardly any discs with solar system building potential would survive this phase. This makes starburst clusters an unlikely environment for the formation of our solar system. Instead it is highly probable that the solar system formed in a leaky cluster (often classified as OB association). We demonstrate that an encounter determining the characteristic properties existing in our solar systems most likely happened very early on (<2 Myr) in its formation history and that after 5 Myr the likelihood of a solar-type star experiencing such an encounter in a leaky cluster is negligible even if it was still part of the bound remnant. This explains why the solar system could develop and maintain its high circularity later in its development.

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Section: Discussionmentioning

confidence: 99%

Early evolution of the birth cluster of the solar system

Pfalzner

2012

A&A

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“…Another hazard for M-stars during the first ∼100 Myr is close stellar flybys, when co-eval stars are still in the expanding cluster of their birth and strongly interacting with each other. During these early close stellar flybys, planetesimals are stripped from disks, and this is more severe for disks around low mass stars in high stellar density clusters like Orion according to simulations (Lestrade et al 2011).…”

Section: ) and Containmentioning

confidence: 98%

A DEBRIS disk around the planet hosting M-star GJ 581 spatially resolved withHerschel

Lestrade

Matthews

Sibthorpe

et al. 2012

A&A

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Debris disks have been found primarily around intermediate and solar mass stars (spectral types A-K) but rarely around low mass M-type stars. We have spatially resolved a debris disk around the remarkable M3-type star GJ 581 hosting multiple planets using deep PACS images at 70, 100 and 160 μm as part of the DEBRIS Program on the Herschel Space Observatory. This is the second spatially resolved debris disk found around an M-type star, after the one surrounding the young star AU Mic (12 Myr). However, GJ 581 is much older (2-8 Gyr), and is X-ray quiet in the ROSAT data. We fit an axisymmetric model of the disk to the three PACS images and found that the best fit model is for a disk extending radially from 25 ± 12 AU to more than 60 AU. Such a cold disk is reminiscent of the Kuiper belt but it surrounds a low mass star (0.3 M ) and its fractional dust luminosity L dust /L * of ∼10 −4 is much higher. The inclination limits of the disk found in our analysis make the masses of the planets small enough to ensure the long-term stability of the system according to some dynamical simulations. The disk is collisionally dominated down to submicron-sized grains and the dust cannot be expelled from the system by radiation or wind pressures because of the low luminosity and low X-ray luminosity of GJ 581. We suggest that the correlation between low-mass planets and debris disks recently found for G-type stars also applies to M-type stars. Finally, the known planets, of low masses and orbiting within 0.3 AU from the star, cannot dynamically perturb the disk over the age of the star, suggesting that an additional planet exists at larger distance that is stirring the disk to replenish the dust.

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“…Another factor contributing to the lack of a well-defined correlation with planet presence might be that the dynamical histories likely vary from system to system, and other stochastic effects need also to be taken into account, e.g., those produced by dynamical instabilities of multiple-planet systems clearing the outer planetesimal belt (Raymond et al 2011(Raymond et al , 2012, the planetesimal belt itself triggering planet migration and instabilities (Tsiganis et al 2005;Levison et al 2011), or the stripping of planetesimals from disks during stellar flybys in the first 100 Myr, when systems are still in their dense birth cluster (Lestrade et al 2011).…”

Section: High-mass Planet Presencementioning

confidence: 99%

DOES THE PRESENCE OF PLANETS AFFECT THE FREQUENCY AND PROPERTIES OF EXTRASOLAR KUIPER BELTS? RESULTS FROM THEHERSCHELDEBRIS AND DUNES SURVEYS

Moro‐Martín

Marshall

Kennedy

et al. 2015

ApJ

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The study of the planet-debris disk connection can shed light on the formation and evolution of planetary systemsand may help "predict" the presence of planets around stars with certain disk characteristics. In preliminary analyses of subsamples of the Herschel DEBRIS and DUNES surveys, Wyatt et al. and Marshall et al. identified a tentative correlation between debris and the presence of low-mass planets. Here we use the cleanest possible sample out of these Herschel surveys to assess the presence of such a correlation, discarding stars without known ages, with ages <1 Gyr, and with binary companions <100 AUto rule out possible correlations due to effects other than planet presence. In our resulting subsample of 204 FGK stars, we do not find evidence that debris disks are more common or more dusty around stars harboring high-mass or low-mass planets compared to a control sample without identified planets. There is no evidence either that the characteristic dust temperature of the debris disks around planet-bearing stars is any different from that in debris disks without identified planets, nor that debris disks are more or less common (or more or less dusty) around stars harboring multiple planets compared to singleplanet systems. Diverse dynamical histories may account for the lack of correlations. The data show a correlation between the presence of high-mass planets and stellar metallicity, but no correlation between the presence of lowmass planets or debris and stellar metallicity. Comparing the observed cumulative distribution of fractional luminosity to those expected from a Gaussian distribution in logarithmic scale, we find that a distribution centered on the solar system's value fits the data well, while one centered at 10 times this value can be rejected. This is of interest in the context of future terrestrial planet detection and characterization because it indicates that there are good prospects for finding a large number of debris disk systems (i.e., with evidence of harboring planetesimals, the building blocks of planets) with exozodiacal emission low enough to be appropriate targets for an ATLASTtype mission to search for biosignatures.

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

Cited by 34 publications

References 55 publications

Early evolution of the birth cluster of the solar system

Early evolution of the birth cluster of the solar system

A DEBRIS disk around the planet hosting M-star GJ 581 spatially resolved withHerschel

DOES THE PRESENCE OF PLANETS AFFECT THE FREQUENCY AND PROPERTIES OF EXTRASOLAR KUIPER BELTS? RESULTS FROM THEHERSCHELDEBRIS AND DUNES SURVEYS

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