Dust production from collisions in extrasolar planetary systems

Thébault, P.; Augereau, J.-C.; Beust, H.

doi:10.1051/0004-6361:20031017

Cited by 96 publications

(141 citation statements)

References 34 publications

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“…This calculation is complicated by the fact that any given debris particle will interact with particles with a range of sizes, with the outcomes of such collisions ranging from cratering to complete pulverisation. For this reason the collisional evolution of debris populations is often studied numerically (Thébault et al 2003;Krivov et al 2005;Bottke et al 2005). However, this is not necessary to understand what happens, because for most common assumptions about collisional outcomes, once the size distribution has reached steady state it tends to a shape that can be readily calculated (O'Brien and Greenberg 2003;Wyatt et al 2011).…”

Section: Collisional Evolutionmentioning

confidence: 99%

Insights into Planet Formation from Debris Disks

Wyatt

Jackson

2016

Space Sci Rev

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Giant impacts refer to collisions between two objects each of which is massive enough to be considered at least a planetary embryo. The putative collision suffered by the proto-Earth that created the Moon is a prime example, though most Solar System bodies bear signatures of such collisions. Current planet formation models predict that an epoch of giant impacts may be inevitable, and observations of debris around other stars are providing mounting evidence that giant impacts feature in the evolution of many planetary systems. This chapter reviews giant impacts, focussing on what we can learn about planet formation by studying debris around other stars. Giant impact debris evolves through mutual collisions and dynamical interactions with planets. General aspects of this evolution are outlined, noting the importance of the collision-point geometry. The detectability of the debris is discussed using the example of the Moon-forming impact. Such debris could be detectable around another star up to 10 Myr post-impact, but model uncertainties could reduce detectability to a few 100 yr window. Nevertheless the 3 % of young stars with debris at levels expected during terrestrial planet formation provide valuable constraints on formation models; implications for super-Earth formation are also discussed. Variability recently observed in some bright disks promises to illuminate the evolution during the earliest phases when vapour condensates may be optically thick and acutely affected by the collision-point geometry. The outer reaches of planetary systems may also exhibit signatures of giant impacts, such as the clumpy debris structures seen around some stars.

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Section: Collisional Evolutionmentioning

confidence: 99%

Insights into Planet Formation from Debris Disks

Wyatt

Jackson

2016

Space Sci Rev

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“…Models of debris disks most often assume a smallest fragment size equal to the blow-out size, s blow (Wyatt & Dent 2002;Wyatt et al 2010), or some constant, but arbitrary, s min < s blow for all collisions (Thébault et al 2003;Krivov et al 2008). The blow-out size corresponds to particles with β = 1/2, L2, page 2 of 5 where…”

Section: Application To Debris Disksmentioning

confidence: 99%

A dearth of small particles in debris disks

Krijt

Kama

2014

A&A

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Context. A prescription for the fragment size distribution resulting from dust grain collisions is essential when modelling a range of astrophysical systems, such as debris disks and planetary rings. Aims. While the slope of the fragment size distribution and the size of the largest fragment are well known, the behaviour of the distribution at the small size end is theoretically and experimentally poorly understood. This leads debris disk codes to generally assume a limit equal to, or below, the radiation blow-out size. Methods. We use energy conservation to analytically derive a lower boundary of the fragment size distribution for a range of collider mass ratios. Focusing on collisions between equal-sized bodies, we apply the method to debris disks. Results. For a given collider mass, the size of the smallest fragments is found to depend on collision velocity, material parameters, and the size of the largest fragment. We provide a physically motivated recipe for the calculation of the smallest fragment, which can be easily implemented in codes for modelling collisional systems. For plausible parameters, our results are consistent with the observed predominance of grains much larger than the blow-out size in Fomalhaut's main belt and in the Herschel cold debris disks.

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“…While the combined effects of material strength and dynamical excitation are thought to dominate the rate of destructive collisions (Thébault et al 2003;Krivov et al 2006), their individual influences differ. The left panel of Fig.…”

Section: Rate and Efficiency Of Collisions Vs Transportmentioning

confidence: 99%

Modelling the huge,Herschel-resolved debris ring around HD 207129

Löhne

Augereau

Ertel

et al. 2012

A&A

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124

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Debris disks, which are inferred from the observed infrared excess to be ensembles of dust, rocks, and probably planetesimals, are common features of stellar systems. As the mechanisms of their formation and evolution are linked to those of planetary bodies, they provide valuable information. The few well-resolved debris disks are even more valuable because they can serve as modelling benchmarks and help resolve degeneracies in modelling aspects such as typical grain sizes and distances. Here, we present an analysis of the HD 207129 debris disk, based on its well-covered spectral energy distribution and Herschel/PACS images obtained in the framework of the DUNES (DUst around NEarby Stars) programme. We use an empirical power-law approach to the distribution of dust and we then model the production and removal of dust by means of collisions, direct radiation pressure, and drag forces. The resulting best-fit model contains a total of nearly 10 −2 Earth masses in dust, with typical grain sizes in the planetesimal belt ranging from 4 to 7 µm. We constrain the dynamical excitation to be low, which results in very long collisional lifetimes and a drag that notably fills the inner gap, especially at 70 µm. The radial distribution stretches from well within 100 AU in an unusual, outward-rising slope towards a rather sharp outer edge at about 170-190 AU. The inner edge is therefore smoother than that reported for Fomalhaut, but the contribution from the extended halo of barely bound grains is similarly small. Both slowly self-stirring and planetary perturbations could potentially have formed and shaped this disk.

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Dust production from collisions in extrasolar planetary systems

Cited by 96 publications

References 34 publications

Insights into Planet Formation from Debris Disks

Insights into Planet Formation from Debris Disks

A dearth of small particles in debris disks

Modelling the huge,Herschel-resolved debris ring around HD 207129

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