The Debris Disk of Vega: A Steady-State Collisional Cascade, Naturally

Müller, Sebastian; Löhne, T.; Krivov, A. V.

doi:10.1088/0004-637x/708/2/1728

Cited by 85 publications

(104 citation statements)

References 73 publications

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“…Such a radial profile that rises outward with a sharp outer edge contrasts with those derived for the archetypal disks Vega (Su et al 2005;Krivov et al 2006;Müller et al 2010;Sibthorpe et al 2010) and β Pictoris (Golimowski et al 2006;Thébault & Wu 2008;Krivov et al 2009;Vandenbussche et al 2010). In these disks, the derived geometrical optical thickness typically falls off with a moderate r −1.5 relationship beyond the peak value, i.e.…”

Section: Resultsmentioning

confidence: 66%

“…The mass depends on the assumed initial size distribution. For collisional equilibrium, κ = −3.0, we would have M(s < 100 km) = 100 Earth masses, a value that is in-between the ones inferred for, e.g., A110, page 12 of 15 Vega (Müller et al 2010) and q 1 Eridani (Augereau et al, in prep.). For κ = −4.0, there would be only M(s < 100 km) = 0.7 Earth masses.…”

Section: Disk Mass and Long-term Evolutionmentioning

confidence: 53%

“…Following the strategy outlined in Müller et al (2010), we start from a first-guess setup based on the roughly known belt location (Krist et al 2010;Marshall et al 2011). After computation of the resulting SED and the radial profiles, we manually alter the most important (and least constrained) disk parameters and re-run the model until we reach a point from where no further significant improvements can be achieved that way.…”

Section: Reference Run and Parameter Variationsmentioning

confidence: 99%

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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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Section: Resultsmentioning

confidence: 66%

Section: Disk Mass and Long-term Evolutionmentioning

confidence: 53%

Section: Reference Run and Parameter Variationsmentioning

confidence: 99%

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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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“…7, having subtracted the 70 µm-attributable component, overplotted with the expected thermal emission from fiducial discs of equal-sized grains with different optical properties, placed at a distance of 130 AU from an F6 V star. A comparison clearly demonstrates that grains smaller than a few tens of micrometres -those that are expected from collisional models (Krivov et al 2006;Thébault & Augereau 2007;Müller et al 2010;Löhne et al 2012) -yield emission that is too warm to be consistent with the observed fluxes. A rough agreement with the observations can only be achieved for larger grains ( > ∼ 1 mm), and only if they have low absorption at optical wavelengths (e.g.…”

Section: Circumstellar Emissionmentioning

confidence: 80%

Herschelobservations of the debris disc around HIP 92043

Marshall¹,

Krivov²,

Burgo³

et al. 2013

A&A

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Context. Typical debris discs are composed of particles ranging from several micron sized dust grains to km sized asteroidal bodies, and their infrared emission peaks at wavelengths 60-100 µm. Recent Herschel DUNES observations have identified several debris discs around nearby Sun-like stars (F, G and K spectral type) with significant excess emission only at 160 µm. Aims. We observed HIP 92043 (110 Her, HD 173667) at far-infrared and sub-millimetre wavelengths with Herschel PACS and SPIRE. Identification of the presence of excess emission from HIP 92043 and the origin and physical properties of any excess was undertaken through analysis of its spectral energy distribution (SED) and the PACS images. Methods. The PACS and SPIRE images were produced using the HIPE photProject map maker routine. Fluxes were measured using aperture photometry. A stellar photosphere model was scaled to optical and near infrared photometry and subtracted from the farinfared and sub-mm fluxes to determine the presence of excess emission. Source radial profiles were fitted using a 2D Gaussian and compared to a PSF model based on Herschel observations of α Boo to check for extended emission. Results. Clear excess emission from HIP 92043 was observed at 70 and 100 µm. Marginal excess was observed at 160 and 250 µm. Analysis of the images reveals that the source is extended at 160 µm. A fit to the source SED is inconsistent with a photosphere and single temperature black body. Conclusions. The excess emission from HIP 92043 is consistent with the presence of an unresolved circumstellar debris disc at 70 and 100 µm, with low probability of background contamination. The extended 160 µm emission may be interpreted as an additional cold component to the debris disc or as the result of background contamination along the line of sight. The nature of the 160 µm excess cannot be determined absolutely from the available data, but we favour a debris disc interpretation, drawing parallels with previously identified cold disc sources in the DUNES sample.

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“…The resulting brightness profiles were convolved with the instrumental PSF (see Sect. 2 in Müller et al 2010, for the algorithm used) and compared them with observed profiles.…”

Section: Surface Brightness Profilesmentioning

confidence: 99%

The cold origin of the warm dust aroundε Eridani

Reidemeister

Krivov

Stark

et al. 2011

A&A

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111

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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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The Debris Disk of Vega: A Steady-State Collisional Cascade, Naturally

Cited by 85 publications

References 73 publications

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

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

Herschelobservations of the debris disc around HIP 92043

The cold origin of the warm dust aroundε Eridani

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