Dusty Debris around Solar‐Type Stars: Temporal Disk Evolution

Spangler, C.; Sargent, Anneila I.; Silverstone, M. D.; Becklin, E. E.; Zuckerman, B.

doi:10.1086/321490

Cited by 167 publications

(238 citation statements)

References 53 publications

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“…The mean fractional dust luminosity,f dust = 1.1 × 10 −3 measured for debris disk in the BPMG, agrees with the expected stage of collisional dust evolution for such ∼12 Myr systems predicted from previous observations (e.g. Su et al 2006;Liu et al 2004;Spangler et al 2001) and models (Kenyon & Bromley 2008;Wyatt et al 2007). The large scatter in f dust among co-eval stars could be a sign of stochastic collisional dust production or a consequence of BMPG's evolutionary stage, perhaps just at the onset of collisional dust cascades at t ≈ 10 Myr.…”

Section: Discussionsupporting

confidence: 88%

A submillimetre search for cold extended debris disks in the $\mathsf{\beta}$ Pictoris moving group

Nilsson

Liseau

Brandeker

et al. 2009

A&A

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Context. Previous observations with the Infrared Astronomical Satellite and the Infrared Space Observatory, and ongoing observations with Spitzer and AKARI, have led to the discovery of over 200 debris disks, based on detected mid-and far infrared excess emission, indicating warm circumstellar dust. To constrain the properties of these systems, e.g., to more accurately determine the dust mass, temperature and radial extent, follow-up observations in the submillimetre wavelength region are needed. Aims. The β Pictoris moving group is a nearby stellar association of young (∼12 Myr) co-moving stars including the classical debris disk star β Pictoris. Due to their proximity and youth, they are excellent targets when searching for submillimetre emission from cold, extended, dust components produced by collisions in Kuiper-Belt-like disks. They also allow an age independent study of debris disk properties as a function of other stellar parameters. Methods. We observed 7 infrared-excess stars in the β Pictoris moving group with the LABOCA bolometer array, operating at a central wavelength of 870 μm at the 12-m submillimetre telescope APEX. The main emission at these wavelengths comes from large, cold dust grains, which constitute the main part of the total dust mass, and hence, for an optically thin case, make better estimates on the total dust mass than earlier infrared observations. Fitting the spectral energy distribution with combined optical and infrared photometry gives information on the temperature and radial extent of the disk. Results. From our sample, β Pic, HD 181327, and HD 172555 were detected with at least 3σ certainty, while all others are below 2σ and considered non-detections. The image of β Pic shows an offset flux density peak located near the south-west extension of the disk, similar to the one previously found by SCUBA at the JCMT. We present SED fits for detected sources and give an upper limit on the dust mass for undetected ones. Conclusions. We find a mean fractional dust luminosityf dust = 1.1 × 10 −3 at t ≈ 12 Myr, which together with recent data at 100 Myr suggests an f dust ∝ t −α decline of the emitting dust, with α > 0.8.

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Section: Discussionsupporting

confidence: 88%

A submillimetre search for cold extended debris disks in the $\mathsf{\beta}$ Pictoris moving group

Nilsson

Liseau

Brandeker

et al. 2009

A&A

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“…Due to the large age uncertainties (represented by horizontal error bars) we refrain from making a fit, and instead only display dashed lines showing the expected decline for three different values of α. We conclude that the temporal evolution of the fractional dust luminosity determined from our observations is in agreement with Nilsson et al (2009), and f dust could perhaps decline as fast as the t −2 found by Spangler et al (2001), although α < 0.8 can not be excluded due to large error bars and small stellar sample. This trend will be better constrained after the completion of the ongoing APEX/LABOCA Large Programme.…”

Section: Temporal Evolution Of Debris Diskssupporting

confidence: 82%

Kuiper belts around nearby stars

Nilsson

Liseau

Brandeker

et al. 2010

A&A

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Context. The existence of dusty debris disks around a large fraction of solar type main-sequence stars, inferred from excess far-IR and submillimetre emission compared to that expected from stellar photospheres, suggests that leftover planetesimal belts analogous to the asteroid-and comet reservoirs of the solar system are common. Aims. Sensitive submillimetre observations are essential to detect and characterise cold extended dust originating from collisions of small bodies in disks, belts, or rings at Kuiper-belt distances (30-50 AU or beyond). Measurements of the flux densities at these wavelengths will extend existing IR photometry and permit more detailed modelling of the Rayleigh-Jeans tail of the disks spectral energy distribution (SED), effectively constraining dust properties and disk extensions. By observing stars spanning from a few up to several hundred Myr, the evolution of debris disks during crucial phases of planet formation can be studied. Methods. We observed 22 exo-Kuiper-belt candidates at 870 μm, as part of a large programme with the LABOCA bolometer at the APEX telescope. Dust masses (or upper limits) were calculated from integrated 870 μm fluxes, and fits to the SED of detected sources revealed the fractional dust luminosities f dust , dust temperatures T dust , and power-law exponents β of the opacity law. Results. A total of 10 detections with at least 3σ significance were made, out of which five (HD 95086, HD 131835, HD 161868, HD 170773, and HD 207129) have previously never been detected at submillimetre wavelengths. Three additional sources are marginally detected with >2.5σ significance. The best-fit β parameters all lie between 0.1 and 0.8, in agreement with previous results indicating the presence of significantly larger grains than those in the ISM. From our relatively small sample we estimate f dust ∝ t −α , with α ∼ 0.8−2.0, and identify an evolution of the characteristic radial dust distance R dust that is consistent with the t 1/3 increase predicted from models of self-stirred collisions in debris disks.

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“…Observational evidence for the presence of disks in clusters of varying ages suggests that (Spangler et al 2001). Only 30% of the members of the NIR cluster are detected in all three bands, and half of those appear to have circumstellar material.…”

Section: Circumstellar Materials Around Members Of the Nir Clustermentioning

confidence: 93%

Discovery of a Massive Protostar near IRAS 18507+0121

Shepherd¹,

Nürnberger²,

Bronfman³

2004

ApJ

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We have observed the massive star-forming region IRAS 18507+0121 at millimeter wavelengths in 3 mm continuum emission, H 13 CO + ( J ¼ 1 0) and SiO (v ¼ 0, J ¼ 2 1) line emission, and at near-infrared (NIR) wavelengths between 1.2 and 2.1 m. Two compact molecular cores are detected: one north and one south, separated by $40 00 . The northern molecular core contains a newly discovered, deeply embedded, B2 protostar surrounded by several hundred solar masses of warm gas and dust, G34.4+0.23 MM. Based on the presence of warm dust emission and the lack of detection at NIR wavelengths, we suggest that G34.4+0.23 MM may represent the relatively rare discovery of a massive protostar (e.g., analogous to a low-mass ''Class 0'' protostar). The southern molecular core is associated with an NIR cluster of young stars and an ultracompact H ii region, G34.4+0.23, with a central B0.5 star. The fraction of NIR stars with excess infrared emission indicative of circumstellar material is greater than 50%, which suggests an upper limit on the age of the IRAS 18507+0121 starforming region of 3 Myr.

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Dusty Debris around Solar‐Type Stars: Temporal Disk Evolution

Cited by 167 publications

References 53 publications

A submillimetre search for cold extended debris disks in the $\mathsf{\beta}$ Pictoris moving group

A submillimetre search for cold extended debris disks in the $\mathsf{\beta}$ Pictoris moving group

Kuiper belts around nearby stars

Discovery of a Massive Protostar near IRAS 18507+0121

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