Modelling the huge,<i>Herschel</i>-resolved debris ring around HD 207129

Löhne, T.; Augereau, J.-C.; Ertel, S.; Marshall, Jonathan P.; Eiroa, C.; Mora, A.; Absil, Olivier; Stapelfeldt, K.; Thébault, P.; Bayo, A.; Burgo, C. del; Danchi, W. C.; Krivov, A. V.; Lebreton, J. P.; Letawe, Géraldine; Magain, Pierre; Maldonado, J.; Montesinos, B.; Pilbratt, G. L.; White, G. J.; Wolf, S.

doi:10.1051/0004-6361/201117731

Cited by 86 publications

(137 citation statements)

References 69 publications

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“…Most of the debris discs that have been observed heretofore have higher dust temperatures and larger fractional luminosities than our own EKB (e.g. q 1 Eri, Liseau et al 2010;HD 207129, A&A 557, A58 (2013) Marshall et al 2011;Löhne et al 2012), a result of the instrumental limitations of current and previous observatories. We present Herschel (Pilbratt et al 2010) PACS (Photodetector Array Camera and Spectrometer, Poglitsch et al 2010) and SPIRE (Spectral and Photometric Imaging REceiver, Griffin et al 2010;Swinyard et al 2010) observations of HIP 92043 (110 Her, HD 173667), a nearby main sequence Sun-like star.…”

Section: Introductionmentioning

confidence: 51%

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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Section: Introductionmentioning

confidence: 51%

Herschelobservations of the debris disc around HIP 92043

Marshall¹,

Krivov²,

Burgo³

et al. 2013

A&A

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“…38, and κ = 0.5 (Löhne et al 2012, and references therein). Table 3 lists all ACE simulations discussed in this paper.…”

Section: Grain Materialsmentioning

confidence: 99%

“…Inspired by the birthring scenario of Strubbe & Chiang (2006), we assumed a radially narrow planetesimal belt centred at a stellocentric distance r PB = 40 au, having the full width ∆r PB = 5 au. In all three runs, the maximum eccentricity of the planetesimals was set to e max = 0.03, motivated by Löhne et al (2012) and Schüppler et al (2014) who showed a preference for low dynamical excitations in debris discs around late-type stars. For the grain material, we chose a homogeneous mixture with volume filled in equal parts by astronomical silicate, amorphous carbon, and vacuum, denoted as M1 (Table 2).…”

Section: Stellar Wind Strengthmentioning

confidence: 99%

“…The scaling factors account for an imperfect reproduction of the total flux density at 1.3 mm, visible by comparing the models with the observed SED. Such imperfections stem, for example, from uncertainties in the absolute flux calibration or in the optical properties of the dust grains (Löhne et al 2012). Furthermore, they derive from a definite inability of our models A97, page 8 of 18 to reproduce the ALMA flux density along with the other photometric data.…”

Section: Impact On Thermal Emissionmentioning

confidence: 99%

“…This makes a total of eight free parameters, R in , R out , α, s min , γ, M d , the dust composition (sampled by only one value, namely 100% astronomical silicate), and the vertical scaling of the ALMA profile. For the fitting of the SED and the ALMA profile, we used the SAnD code (Ertel et al 2012a;Löhne et al 2012), which was originally developed for fitting simultaneously SED data and spatially resolved Herschel data as part of the Herschel/DUNES modelling tool box. We did not include the scattered light data for this power-law fitting.…”

Section: Comparison With Parametric Modellingmentioning

confidence: 99%

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Collisional modelling of the AU Microscopii debris disc

Schüppler

Löhne

Krivov

et al. 2015

A&A

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AU Microscopii's debris disc is one of the most famous and best-studied debris discs and one of only two resolved debris discs around M stars. We perform in-depth collisional modelling of the AU Mic disc including stellar radiative and corpuscular forces (stellar winds), aiming at a comprehensive understanding of the dust production and the dust and planetesimal dynamics in the system. Our models are compared to a suite of observational data for thermal and scattered light emission, ranging from the ALMA radial surface brightness profile at 1.3 mm to spatially resolved polarisation measurements in the visible. Most of the data are shown to be reproduced with dust production in a belt of planetesimals with an outer edge at around 40 au and subsequent inward transport of dust by stellar winds. A low dynamical excitation of the planetesimals with eccentricities up to 0.03 is preferred. The radial width of the planetesimal belt cannot be constrained tightly. Belts that are 5 au and 17 au wide, as well as a broad 44 au-wide belt, are consistent with observations. All models show surface density profiles that increase with distance from the star up to ≈40 au, as inferred from observations. The best model is achieved by assuming a stellar mass loss rate that exceeds the solar one by a factor of 50. The models reproduce the spectral energy distribution and the shape of the ALMA radial profile well, but deviate from the scattered light observations more strongly. The observations show a bluer disc colour and a lower degree of polarisation for projected distances <40 au than predicted by the models. These deviations may be reduced by taking irregularly shaped dust grains which have scattering properties different from the Mie spheres used in this work. From tests with a handful of selected dust materials, we favour mixtures of silicate, carbon, and ice of moderate porosity. We also address the origin of the unresolved central excess emission detected by ALMA and show that it cannot stem from an additional inner belt alone. Instead, it should derive, at least partly, from the chromosphere of the central star.

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Debris disks as seen by Herschel/DUNES

et al. 2012

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The far-infrared excesses produced by debris disks are common features of stellar systems. These disks are thought to contain solids ranging from micron-sized dust to planetesimals. Naturally, their formation and evolution are linked to those of potential planets. With this motivation, the Herschel open time key programme DUNES (DUst around NEarby Stars) aims at further characterising known debris disks and discovering new ones in the regime explored by the Herschel space observatory. On the one hand, in their survey of 133 nearby FGK stars, DUNES discovered a class of extremely cold and faint debris disks, different from well-known disks such as the one around Vega in that their inferred typical grain sizes are rather large, indicating low dynamical excitation and low collision rates. On the other hand, for the more massive disk around the sun-like star HD 207129, well-resolved PACS images confirmed the ring-liked structure seen in HST images and provided valuable information for an in-depth study and benchmark for models. Employing both models for power-law fitting and collisional evolution we found the disk around HD 207129 to feature low collision rates and large grains, as well. Transport by means of Poynting-Robertson drag likely plays a role in replenishing the dust seen closer to the star, inside of the ring. The inner edge is therefore rather smooth and the contribution from the extended halo of barely bound grains is small. Both slowly self-stirring and planetary perturbations could potentially have formed and shaped this disk.

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

Cited by 86 publications

References 69 publications

Herschelobservations of the debris disc around HIP 92043

Herschelobservations of the debris disc around HIP 92043

Collisional modelling of the AU Microscopii debris disc

Debris disks as seen by Herschel/DUNES

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