An unbiased study of debris discs around A-type stars with Herschel

Thureau, N.; Greaves, J. S.; Matthews, Brenda C.; Kennedy, Grant M.; Phillips, Neil; Booth, Mark; Duchêne, Gaspard; Horner, Jonathan; Rodríguez, David; Sibthorpe, B.; Wyatt, M. C.

doi:10.1093/mnras/stu1864

Cited by 124 publications

(98 citation statements)

References 63 publications

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“…Within the gas disk we derive an excitation temperature of T 0 = 27 -+ 4 11 K. Spitzer observations find typical dust temperatures of 50-200 K in debris disks (Morales et al 2011;Ballering et al 2013), with similar results found by Herschel (Matthews et al 2010;Eiroa et al 2013;Thureau et al 2014), although this depends strongly on the location and composition of the dust grains. In debris disks the dust temperature at a given radius is often found to be higher than that for blackbody grains, or conversely the observed radial location of the dust grains is larger than predicted for blackbody grains (Booth et al 2013).…”

Section: Discussionsupporting

confidence: 86%

Resolved Co Gas Interior to the Dust Rings of the Hd 141569 Disk

Flaherty

Hughes

Andrews

et al. 2016

ApJ

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The disk around HD 141569 is one of a handful of systems whose weak infrared emission is consistent with a debris disk, but still has a significant reservoir of gas. Here we report spatially resolved millimeter observations of the CO(3-2) and CO(1-0) emission as seen with the Submillimeter Array and CARMA. We find that the excitation temperature for CO is lower than expected from cospatial blackbody grains, similar to previous observations of analogous systems, and derive a gas mass that lies between that of gas-rich primordial disks and gas-poor debris disks. The data also indicate a large inner hole in the CO gas distribution and an outer radius that lies interior to the outer scattered light rings. This spatial distribution, with the dust rings just outside the gaseous disk, is consistent with the expected interactions between gas and dust in an optically thin disk. This indicates that gas can have a significant effect on the location of the dust within debris disks.

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Section: Discussionsupporting

confidence: 86%

Resolved Co Gas Interior to the Dust Rings of the Hd 141569 Disk

Flaherty

Hughes

Andrews

et al. 2016

ApJ

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“…A KS test reveals no difference between single and multiple stars in terms of dust temperature (p=0.9) or LIR/L bol (p=0.5), as was also demonstrated for A stars by Thureau et al (2014). This holds regardless of whether we consider the full sample or break it as A or FGK stars: for dust temperatures we find p=0.3 for A singles vs multiples and similarly p=0.9 for FGK systems.…”

Section: Global Statisticssupporting

confidence: 67%

“…Disk systems among the sample are summarized in Matthews et al (in prep), Thureau et al (2014), and Sibthorpe et al (in prep). Despite the large number of systems considered, the number of disk-bearing systems (78 across all spectral types) is lower than considered in Rodriguez & Zuckerman (2012).…”

Section: Discussionmentioning

confidence: 99%

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Stellar multiplicity and debris discs: an unbiased sample

Rodríguez

Duchêne

Tom

et al. 2015

Monthly Notices of the Royal Astronomical Society

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Circumstellar dust disks have been observed around many nearby stars. However, many stars are part of binary or multiple stellar systems. A natural question arises regarding the presence and properties of such disks in systems with more than one star. To address this, we consider a sample of 449 systems (spectral types A-M) observed with the Herschel Space Observatory as part of the DEBRIS program. We have examined the stellar multiplicity of this sample by gathering information from the literature and performing an adaptive optics imaging survey at Lick Observatory. Five new companions were revealed with our program. In total, we identify 188 (42%) binary or multiple star systems. The multiplicity of the sample is examined with regards to the detection of circumstellar disks for stars of spectral types AFGK.In general, disks are less commonly detected around binaries than single stars, though the disk frequency is comparable among A stars regardless of multiplicity. However, this sample reveals the period distribution of disk-bearing binaries is consistent with that of non-disk binaries and with comparison field samples. We find that the properties of disks in binary systems are not statistically different from those around single stars. Although the frequency of disk-bearing FGK binaries may be lower than in single star systems, the processes behind disk formation and the characteristics of these disks are comparable among both populations.

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“…Data used 2.1. Stellar properties AU Mic (GJ 803, HD 197481) is an M1 V dwarf at a distance of 9.9 pc (Perryman et al 1997;van Leeuwen 2007). The star is a bright X-ray and UV emitter and shows strong flaring activity (e.g., Robinson et al 2001).…”

Section: Introductionmentioning

confidence: 99%

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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An unbiased study of debris discs around A-type stars with Herschel

Cited by 124 publications

References 63 publications

Resolved Co Gas Interior to the Dust Rings of the Hd 141569 Disk

Resolved Co Gas Interior to the Dust Rings of the Hd 141569 Disk

Stellar multiplicity and debris discs: an unbiased sample

Collisional modelling of the AU Microscopii debris disc

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