Collisional processes and size distribution  in spatially extended debris discs

Thébault, P.; Augereau, J.-C.

doi:10.1051/0004-6361:20077709

Cited by 158 publications

(270 citation statements)

References 58 publications

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“…Generally speaking, these are in the 0.1-5 µm range and in good agreement with the expected blow-out size given the central star luminosity and/or stellar wind (Boccaletti et al, 2003;Clampin et al, 2003;Golimowski et al, 2006;Kalas et al, 2007a). It is arguable whether a strict power-law size distribution should be expected in a collisional cascade (Thébault and Augereau, 2007). Here, scattered light images at multiple wavelengths can provide constraints for the grain size distribution.…”

Section: Inner Disk Regions: Observational Findingssupporting

confidence: 61%

Circumstellar disks and planets

Wolf

Malbet

Alexander

et al. 2012

Astron Astrophys Rev

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We present a review of the interplay between the evolution of circumstellar disks and the formation of planets, both from the perspective of theoretical models and dedicated observations. Based on this, we identify and discuss fundamental questions concerning the formation and evolution of circumstellar disks and planets which can be addressed in the near future with optical and infrared long-baseline interferometers. Furthermore, the importance of complementary observations with long-baseline (sub)millimeter interferometers and high-sensitivity infrared observatories is outlined.

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Section: Inner Disk Regions: Observational Findingssupporting

confidence: 61%

Circumstellar disks and planets

Wolf

Malbet

Alexander

et al. 2012

Astron Astrophys Rev

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“…We do not observe here the "wavy" size distribution, starting at the blow-out size (β ∼ 0.5) imposed by radiation pressure, expected in realistic collisional systems (Thébault & Augereau 2007). This is because our expression for t coll is too simplified to account for such complex effects.…”

Section: Size Distribution In the Parent Body Regionmentioning

confidence: 68%

“…Figure 5 should thus be regarded as a first approximation. However, to check the robustness of our results we performed a test run using the t coll expression of Thébault & Augereau (2007) for the e b = 0.3 companion case. We verify that, even for this highly unrealistic case artificially forcing an effect at the β = 0.5 limit, the resulting size distribution is remarkably similar to that of Fig.…”

Section: Size Distribution In the Parent Body Regionmentioning

confidence: 99%

“…This corresponds in practice to astrophysical cases with greater binary separation, where the companion star did not 6 When using the expression of Thébault & Augereau (2007) instead of our Eq. (2) in the non-perturbed single-star case, we do indeed obtain a pronounced wavy pattern for the size distribution truncate the initial protoplanetary ring and a out is the natural disc outer limit.…”

Section: Inner Ring Casementioning

confidence: 99%

“…A e p ≤ 0.01 solution is thus possible in principle, but it might not hold from a theoretical point of view. Debris discs are indeed systems in which the bulk of planetesimal accretion process should already be over, and planets or planetary embryos are present and dynamically excite all remaining particles to eccentricities in the 0.05-0.1 range (Artymowicz 1997;Thébault & Augereau 2007). As an example, Wyatt et al (1999) assume e p = 0.13 for their model of the HR4796A disc.…”

Section: Resolved Observations: Hr4796mentioning

confidence: 99%

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Debris discs in binaries: a numerical study

Thébault

Marzari

Augereau

2010

A&A

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Context. Debris disc analysis and modelling provide crucial information about the structure and the processes at play in extrasolar planetary systems. In binary systems, this issue is more complex because the disc should also respond to the companion star's perturbations. Aims. We explore the dynamical evolution of a collisionally active debris disc for different initial parent body populations, diverse binary configurations, and optical depths. We focus on the radial extent and size distribution of the disc in a stationary state. Methods. We numerically followed the evolution of 10 5 massless small grains, initially produced from a circumprimary disc of parent bodies following a size distribution in dN ∝ s −3.5 ds . Grains were submitted to both stars' gravity and radiation pressure. In addition, particles were assigned an empirically derived collisional lifetime. Results. For all the binary configurations, the disc extends far beyond the critical semi-major axis a crit for orbital stability. This is due to the steady production of small grains, placed by radiation pressure on eccentric orbits reaching beyond a crit . The amount of matter beyond a crit depends on the balance between collisional production and dynamical removal rates: it increases for more massive discs, as well as for eccentric binaries. Another important effect is that, in the dynamically stable region, the disc is depleted from its smallest grains. Both results could lead to observable signatures. Conclusions. We have shown that a companion star can never fully truncate a collisionally active disc. For eccentric companions, grains in the unstable regions can contribute significantly to the thermal emission in the mid-IR. Discs with sharp outer edges, especially bright ones such as HR4796A, are probably shaped by other mechanisms.

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Dynamics of Small Bodies in Planetary Systems

Wyatt

2008

Small Bodies in Planetary Systems

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The number of stars that are known to have debris disks is greater than that of stars known to harbour planets. These disks are detected because dust is created in the destruction of planetesimals in the disks much in the same way that dust is produced in the asteroid belt and Kuiper belt in the solar system. For the nearest stars the structure of their debris disks can be directly imaged, showing a wide variety of both axisymmetric and asymmetric structures. A successful interpretation of these images requires a knowledge of the dynamics of small bodies in planetary systems, since this allows the observed dust distribution to be deconvolved to provide information on the distribution of larger objects, such as planetesimals and planets. This chapter reviews the structures seen in debris disks, and describes a disk dynamical theory which can be used to interpret those observations. In this way much of the observed structures, both axisymmetric and asymmetric, can be explained by a model in which the dust is produced in a planetesimal belt which is perturbed by a nearby, as yet unseen, planet. While the planet predictions still require confirmation, it is clear that debris disks have the potential to provide unique information about the structure of extrasolar planetary systems, since they can tell us about planets analogous to Neptune and even the Earth. Significant failings of the model at present are its inability to predict the quantity of small grains in a system, and to explain the origin of the transient dust seen in some systems. Given the complexity of planetary system dynamics and how that is readily reflected in the structure of a debris disk, it seems inevitable that the study of debris disks will play a vital role in our understanding of extrasolar planetary systems.

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Collisional processes and size distribution in spatially extended debris discs

Cited by 158 publications

References 58 publications

Circumstellar disks and planets

Circumstellar disks and planets

Debris discs in binaries: a numerical study

Dynamics of Small Bodies in Planetary Systems

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