Herschel Observations of Dusty Debris Disks

Vican, Laura; Schneider, Adam C.; Bryden, G.; Melis, Carl; Zuckerman, B.; Rhee, J.; Song, Inseok

doi:10.3847/1538-4357/833/2/263

Cited by 46 publications

(21 citation statements)

References 77 publications

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“…In July 2011 and January 2012, the Herschel Space Observatory used its Photodetector Array Camera and Spectrometer (PACS) to measure BD +20 307 at 70 and 100 µm. The reported 70 µm flux density of 47 ± 3 mJy (Vican et al 2016) is substantially larger than that reported with MIPS from 2007 of 28.6 ± 1.9 mJy (Weinberger et al 2011).…”

Section: Previous Observationscontrasting

confidence: 70%

Studying the Evolution of Warm Dust Encircling BD +20 307 Using SOFIA

Thompson

Weinberger²,

Keller

et al. 2019

ApJ

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The small class of known stars with unusually warm, dusty debris disks is a key sample to probe in order to understand cascade models and extreme collisions that likely lead to the final configurations of planetary systems. Because of its extreme dustiness and small radius, the disk of BD +20 307 has a short predicted collision time and is therefore an interesting target in which to look for changes in dust quantity and composition over time. To compare with previous ground and Spitzer Space Telescope data, SOFIA photometry and spectroscopy were obtained. The system's 8.8-12.5 µm infrared emission increased by 10 ± 2% over nine years between the SOFIA and earlier Spitzer measurements. In addition to an overall increase in infrared excess, there is a suggestion of a greater increase in flux at shorter wavelengths (less than 10.6 µm) compared to longer wavelengths (greater than 10.6 µm). Steady-state collisional cascade models cannot explain the increase in BD +20 307's disk flux over such short timescales. A catastrophic collision between planetary-scale bodies is still the most likely origin for the system's extreme dust; however, the cause for its recent variation requires further investigation.

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Section: Previous Observationscontrasting

confidence: 70%

Studying the Evolution of Warm Dust Encircling BD +20 307 Using SOFIA

Thompson

Weinberger²,

Keller

et al. 2019

ApJ

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“…Allowing for the superheat ratio T obs /T BB = 100K/71K = 1.41 found by NIRDS for dust in the HR 4796A (A0.5V) ring at ~75 AU from its primary (Lisse et al 2017) moves this location out to ~40 AU, closer to the Curie et al estimate. The remaining discrepancy between the spectral and imaging radial distance estimates might be due to our poor current characterization of the MIR-FIR SED peak; to our lack of understanding of the superheat behavior of the HD 36546 outer dust (values of T obs /T BB out to [5][6][7][8][9][10][11][12][13][14][15] have been reported by Rodriguez &Zuckerman 2012 andVican et al 2016) ; or to the different sensitivities of scattered light (∝ surface area*albedo) vs. thermal emission (∝ surface area*emissivity*T 4 ) measurements of circumstellar dust in a thick disk, which will weight closer-in dust thermal emission most highly (c.f. Watson et al 2009 and references therein).…”

Section: Discussionmentioning

confidence: 99%

Spectral Evidence for an Inner Carbon-rich Circumstellar Belt in the Young HD 36546 A-star System

Lisse

Sitko

Russell

et al. 2017

ApJL

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Using the NASA/IRTF SpeX & BASS spectrometers we have obtained 0.7 -13 µm observations of the newly imaged HD36546 debris disk system. The SpeX spectrum is most consistent with the photospheric emission expected from an L * ~ 20 L ! , solar abundance A1.5V star with little to no extinction, and excess emission from circumstellar dust detectable beyond 4.5 µm. Non-detections of CO emission lines and accretion signatures point to the gas-poor circumstellar environment of a very old transition disk. Combining the SpeX + BASS spectra with archival WISE/AKARI/IRAS/Herschel photometry, we find an outer cold dust belt at ~135K and 20-40 AU from the primary, likely coincident with the disk imaged by Subaru (Currie et al. 2017), and a new second inner belt with temperature ~570K and an unusual, broad SED maximum in the 6-9 µm region, tracing dust at 1.1-2.2 AU. An SED maximum at 6-9 µm has been reported in just two other A-star systems, HD131488 and HD121191, both of ~10 Myr age (Melis et al. 2013). From Spitzer, we have also identified the ~12 Myr old A7V HD148567 system as having similar 5 -35 µm excess spectral features (Mittal et al. 2015). The Spitzer data allows us to rule out water emission and rule in carbonaceous materials -organics, carbonates, SiC -as the source of the 6-9 µm excess. Assuming a common origin for the 4 young A-star systems' disks, we suggest they are experiencing an early era of carbon-rich planetesimal processing.

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“…This criterion is certainly met by cool Edgeworth-Kuiper belt analogues, but falls down for stars at an earlier evolutionary phase where planet formation is believed to be ongoing, and where the flux excess tends to peak at mid-IR wavelengths (e.g. Melis et al 2010;Fujiwara et al 2012;Vican et al 2016). The fractional luminosities for the SONS surveys discs are given in Table 3, and all but beam in arcseconds, then the disc radius as specified in Equation 2 will be in astronomical units.…”

Section: Fractional Luminositiesmentioning

confidence: 99%

SONS: The JCMT legacy survey of debris discs in the submillimetre

Holland

Matthews

Kennedy

et al. 2017

Monthly Notices of the Royal Astronomical Society

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128

111

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Debris discs are evidence of the ongoing destructive collisions between planetesimals, and their presence around stars also suggests that planets exist in these systems. In this paper, we present submillimetre images of the thermal emission from debris discs that formed the SCUBA-2 Observations of Nearby Stars (SONS) survey, one of seven legacy surveys undertaken on the James Clerk Maxwell telescope between 2012 and 2015. The overall results of the survey are presented in the form of 850 µm (and 450 µm, where possible) images and fluxes for the observed fields. Excess thermal emission, over that expected from the stellar photosphere, is detected around 49 stars out of the 100 observed fields. The discs are characterised in terms of their flux density, size (radial distribution of the dust) and derived dust properties from their spectral energy distributions. The results show discs over a range of sizes, typically 1-10 times the diameter of the Edgeworth-Kuiper Belt in our Solar System. The mass of a disc, for particles up to a few millimetres in size, is uniquely obtainable with submillimetre observations and this quantity is presented as a function of the host stars' age, showing a tentative decline in mass with age. Having doubled the number of imaged discs at submillimetre wavelengths from ground-based, single dish telescope observations, one of the key legacy products from the SONS survey is to provide a comprehensive target list to observe at high angular resolution using submillimetre/millimetre interferometers (e.g., ALMA, SMA).

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Herschel Observations of Dusty Debris Disks

Cited by 46 publications

References 77 publications

Studying the Evolution of Warm Dust Encircling BD +20 307 Using SOFIA

Studying the Evolution of Warm Dust Encircling BD +20 307 Using SOFIA

Spectral Evidence for an Inner Carbon-rich Circumstellar Belt in the Young HD 36546 A-star System

SONS: The JCMT legacy survey of debris discs in the submillimetre

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