The Edgeworth-Kuiper debris disk

Vitense, Ch.; Krivov, A. V.; Löhne, T.

doi:10.1051/0004-6361/201014208

Cited by 55 publications

(78 citation statements)

References 83 publications

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“…This is close to what is expected theoretically for collision-dominated disks (Dohnanyi 1969). However, from s c ≈ 10 μm down to the smallest grains, the size distribution flattens, because the inward drift is faster for smaller grains -or, more exactly, for grains with higher β-ratios (see, e.g., Strubbe & Chiang 2006;Vitense et al 2010, for a more detailed discussion of this phenomenon). The slope calculated analytically for a transport-dominated disk with β ∝ s −1 is q ≈ 2.5.…”

Section: Resultssupporting

confidence: 87%

The cold origin of the warm dust aroundε Eridani

Reidemeister

Krivov

Stark

et al. 2011

A&A

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Context. The nearby K2 V star ε Eridani hosts one known inner planet, an outer Kuiper belt analog, and an inner disk of warm dust. Spitzer/IRS measurements indicate that the warm dust is present at distances as close as a few AU from the star. Its origin is puzzling, since an "asteroid belt" that could produce this dust would be unstable because of the known inner planet. Aims. Here we test a hypothesis that the observed warm dust is generated by collisions in the outer belt and is transported inward by Poynting-Robertson drag and strong stellar winds. Methods. We simulated a steady-state distribution of dust particles outside 10 AU with a collisional code and in the inner region (r < 10 AU) with single-particle numerical integrations. By assuming homogeneous spherical dust grains composed of ice and astrosilicate, we calculated the thermal emission of the dust and compared it with observations. We investigated two different orbital configurations for the inner planet inferred from radial velocity measurements, one with a highly eccentric orbit of e = 0.7 and another one with a moderate eccentricity of e = 0.25. We also produced a simulation without a planet. Results. Our models can reproduce the shape and magnitude of the observed spectral energy distribution from mid-infrared to submillimeter wavelengths, as well as the Spitzer/MIPS radial brightness profiles. The best-fit dust composition includes both water ice and silicates. The results are similar for the two possible planetary orbits and without a planet. Conclusions. The observed warm dust in the ε Eridani system can indeed stem from the outer "Kuiper belt" and be transported inward by Poynting-Robertson and stellar wind drag. The inner planet has little effect on the distribution of dust, so that the planetary orbit could not be constrained. Reasonable agreement between the model and observations can only be achieved by relaxing the assumption of purely silicate dust and assuming a mixture of silicate and water ice in comparable amounts.

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Section: Resultssupporting

confidence: 87%

The cold origin of the warm dust aroundε Eridani

Reidemeister

Krivov

Stark

et al. 2011

A&A

Self Cite

111

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“…Strubbe & Chiang (2006) derive the theoretical values of α = 1.5 and α = 2.5 for collision and P-R drag-dominated disks, respectively. We find slopes of α ≈ 2.0 for both runs, consistent with the outer slope found by Vitense et al (2010) for the Edgeworth-Kuiper Belt, and interpreted as the sign of a disk that is in between drag and collision-dominated. This indicates that the density of the parent belt (characterized by η 0 ∼ 10) is insufficient to make the outer disk completely collision-dominated.…”

Section: Radial Distributionsupporting

confidence: 88%

Near-infrared emission from sublimating dust in collisionally active debris disks

Lieshout

Dominik

Kama

et al. 2014

A&A

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Context. Hot exozodiacal dust is thought to be responsible for excess near-infrared (NIR) emission emanating from the innermost parts of some debris disks. The origin of this dust, however, is still a matter of debate. Aims. We test whether hot exozodiacal dust can be supplied from an exterior parent belt by Poynting-Robertson (P-R) drag, paying special attention to the pile-up of dust that occurs owing to the interplay of P-R drag and dust sublimation. Specifically, we investigate whether pile-ups still occur when collisions are taken into account, and if they can explain the observed NIR excess. Methods. We computed the steady-state distribution of dust in the inner disk by solving the continuity equation. First, we derived an analytical solution under a number of simplifying assumptions. Second, we developed a numerical debris disk model that for the first time treats the complex interaction of collisions, P-R drag, and sublimation in a self-consistent way. From the resulting dust distributions, we generated thermal emission spectra and compare these to observed excess NIR fluxes. Results. We confirm that P-R drag always supplies a small amount of dust to the sublimation zone, but find that a fully consistent treatment yields a maximum amount of dust that is about 7 times lower than that given by analytical estimates. The NIR excess due to this material is much less ( < ∼ 10 −3 for A-type stars with parent belts at > ∼ 1 AU) than the values derived from interferometric observations (∼10 −2 ). Pile-up of dust still occurs when collisions are considered, but its effect on the NIR flux is insignificant. Finally, the cross-section in the innermost regions is clearly dominated by barely bound grains.

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“…In our previous paper (Vitense et al 2010), we took the current database of known trans-Neptunian objects (TNOs) and employed a new algorithm to eliminate the inclination and the distance selection effects in the known TNO populations and derived expected parameters of the "true" EKB. Treating the debiased populations of EKB objects as dust parent bodies, we then produced their dust disk with our collisional code.…”

Section: Introductionmentioning

confidence: 99%

“…The main goal of this paper is to improve the model by Vitense et al (2010) in several important respects:…”

Section: Introductionmentioning

confidence: 99%

An improved model of the Edgeworth-Kuiper debris disk

Vitense

Krivov

Kobayashi

et al. 2012

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In contrast to all other debris disks, where the dust can be seen via an infrared excess over the stellar photosphere, the dust emission of the Edgeworth-Kuiper belt (EKB) eludes remote detection because of the strong foreground emission of the zodiacal cloud. We accessed the expected EKB dust disk properties by modeling. We treated the debiased population of the known trans-Neptunian objects (TNOs) as parent bodies and generated the dust with our collisional code. The resulting dust distributions were modified to take into account the influence of gravitational scattering and resonance trapping by planets on migrating dust grains as well as the effect of sublimation. A difficulty with the modeling is that the amount and distribution of dust are largely determined by sub-kilometer-sized bodies. These are directly unobservable, and their properties cannot be accessed by collisional modeling, because objects larger than (10 . . . 60) m in the present-day EKB are not in a collisional equilibrium. To place additional constraints, we used in-situ measurements of the New Horizons spacecraft within 20 AU. We show that to sustain a dust disk consistent with these measurements, the TNO population has to have a break in the size distribution at s 70 km. However, even this still leaves us with several models that all correctly reproduce nearly constant dust impact rates in the region of giant planet orbits and do not violate the constraints from the non-detection of the EKB dust thermal emission by the COBE spacecraft. The modeled EKB dust disks, which conform to the observational constraints, can either be transport-dominated or intermediate between the transport-dominated and collision-dominated regime. The in-plane optical depth of such disks is τ (r > 10 AU) ∼ 10 −6 and their fractional luminosity is f d ∼ 10 −7 . Planets and sublimation are found to have little effect on dust impact fluxes and dust thermal emission. The spectral energy distribution of an EKB analog as seen from 10 pc distance peaks at wavelengths of (40 . . . 50) µm at F ≈ 0.5 mJy, which is less than 1% of the photospheric flux at those wavelengths. Therefore, EKB analogs cannot be detected with present-day instruments such as Herschel/PACS.

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The Edgeworth-Kuiper debris disk

Cited by 55 publications

References 83 publications

The cold origin of the warm dust aroundε Eridani

The cold origin of the warm dust aroundε Eridani

Near-infrared emission from sublimating dust in collisionally active debris disks

An improved model of the Edgeworth-Kuiper debris disk

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