Zodiacal Dust Bands

Dermott, S. F.; Durda, D. D.; Gustafson, B. Å. S.; Jayaraman, S.; Liou, J.‐C.; Xu, Y. L.

doi:10.1007/978-94-011-1148-5_10

Cited by 44 publications

(38 citation statements)

References 23 publications

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“…The 3σ limits on L dust /L at 8.5-12 μm and 30-34 μm have 2σ clipped average values of L dust /L = 11 ± 4 × 10 −5 and 1.31 ± 0.49 × 10 −5 , respectively (Table 4). In comparison with our solar system, which has L dust /L ∼ 10 −7 (Backman & Paresce 1993;Dermott et al 2002), the IRS results set limits (3σ ) on warm (360 K) dust peaking at 10 μm of ∼1000 times the level of dust emission in our solar system. For cooler dust (∼115 K) peaking at 30-34 μm, the 3σ limit corresponds to ∼100 times the nominal L dust /L of our zodiacal cloud.…”

Section: Limits On the Fractional Disk Luminositysupporting

confidence: 59%

EXPLORATIONS BEYOND THE SNOW LINE:SPITZER/IRS SPECTRA OF DEBRIS DISKS AROUND SOLAR-TYPE STARS

Lawler

Beichman

Bryden

et al. 2009

ApJ

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We have observed 152 nearby solar-type stars with the Infrared Spectrometer (IRS) on the Spitzer Space Telescope. Including stars that met our criteria but were observed in other surveys, we get an overall success rate for finding excesses in the long-wavelength IRS band (30-34 μm) of 11.8% ± 2.4%. The success rate for excesses in the shortwavelength band (8.5-12 μm) is ∼1% including sources from other surveys. For stars with no excess at 8.5-12 μm, the IRS data set 3σ limits of around 1000 times the level of zodiacal emission present in our solar system, while at 30-34 μm data set limits of around 100 times the level of our solar system. Two stars (HD 40136 and HD 10647) show weak evidence for spectral features; the excess emission in the other systems is featureless. If the emitting material consists of large (10 μm) grains as implied by the lack of spectral features, we find that these grains are typically located at or beyond the snow line, ∼1-35 AU from the host stars, with an average distance of 14 ± 6 AU; however, smaller grains could be located at significantly greater distances from the host stars. These distances correspond to dust temperatures in the range ∼50-450 K. Several of the disks are well modeled by a single dust temperature, possibly indicative of a ring-like structure. However, a single dust temperature does not match the data for other disks in the sample, implying a distribution of temperatures within these disks. For most stars with excesses, we detect an excess at both IRS and Multiband Imaging Photometer for Spitzer (MIPS) wavelengths. Only three stars in this sample show a MIPS 70 μm excess with no IRS excess, implying that very cold dust is rare around solar-type stars.

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Section: Limits On the Fractional Disk Luminositysupporting

confidence: 59%

EXPLORATIONS BEYOND THE SNOW LINE:SPITZER/IRS SPECTRA OF DEBRIS DISKS AROUND SOLAR-TYPE STARS

Lawler

Beichman

Bryden

et al. 2009

ApJ

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“…The traditional view of debris discs is that of a ring of planetesimals residing outside any planetary system producing cold dust, analogous to the Edgeworth-Kuiper belt (EKB) in the Solar System. Multiple component discs could be seen as analogous to the Solar System, although of course the extrasolar discs detected to date are much brighter than the asteroid belt and EKB (L IR /L ≥ 10 −4 for detected extrasolar discs; asteroid and Edgeworth-Kuiper belts L IR /L = 10 −8 −10 −7 and 10 −7 −10 −6 respectively, Dermott et al 2002b;Stern & Colwell 1997).…”

Section: Discussionmentioning

confidence: 93%

“…We therefore calculate the detectability of exozodiacal emission by assuming this is equivalent to the detectability of a ring at the optimal radius. Taking the optical depth of the zodiacal cloud, τ = 5 × 10 −8 (Dermott et al 2002a), and assuming a ring of width dr = 0.5r gives a fractional luminosity of f = 0.5(dr/r)τ = 1.25×10 −8 . If we consider a sunlike star at 10 pc, the optimal detection radius would be centered at r = 0.5 AU.…”

Section: Metis On the E-eltmentioning

confidence: 99%

Warm dusty discs: exploring the A star 24 μm debris population

Smith¹,

Wyatt

2010

A&A

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Aims. Studies of the debris disc phenomenon have shown that most systems are analogous to the Edgeworth-Kuiper belt (EKB). In this study we aim to determine how many of the IRAS 25 μm excesses towards A stars, which may be indicative of asteroid belt analogues, are real, and investigate where the dust must lie and so build up a picture of what these systems are like. Methods. We observe using ground-based mid-infrared imaging with TIMMI2, VISIR, Michelle and TReCS a sample of A and B-type main sequence stars previously reported as having mid-infrared excess. We combine modelling of the emission spectrum from multi-wavelength photometry with a modelling technique designed to constrain the radial extent of emission in mid-infrared imaging to constrain the possible location of the debris. Results. We independently confirm the presence of warm dust around three of the candidates: HD 3003, HD 80950 and η Tel. For the binary HD3003 a stability analysis indicates the dust is either circumstellar and lying at ∼4 AU with the binary orbiting at >14 AU, or the dust lies in an unstable location; there is tentative evidence for temporal evolution of its excess emission on a ∼20 year timescale. For 7 of the targets we present quantitative limits on the location of dust around the star based on the unresolved imaging. We demonstrate that the disc around HD71155 must have multiple spatially distinct components at 2 and 60 AU. We model the limits of current instrumentation to resolve debris disc emission and show that most of the known A star debris discs which could be readily resolved at 18 μm on 8 m instruments have been resolved, but identify several that could be resolved with deep (>8 h total) integrations (such as HD19356, HD139006 and HD102647). Conclusions. Limits from unresolved imaging can help distinguish between competing models of the disc emission, but resolved imaging is key to an unambiguous determination of the disc location. Modelling of the detection limits for extended emission can be useful for targeting future observational campaigns towards sources most likely to be resolved. MIRI on the JWST will be able to resolve the majority of the known A star debris disc population. METIS on the E-ELT will provide the opportunity to explore the hot disc population more thoroughly by detecting extended emission down to where calibration accuracy limits disc detection through photometry alone, reaching levels below 1 zodi for stars within 10 pc.

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“…It is thought that due to the depletion of asteroids, the asteroidal dust surface area has slowly declined by a factor of 10 ) with excursions in the dust production rate by up to an order of magnitude associated with breakup events like those giving rise to the Hirayama asteroid families that resulted in the formation of the dust bands observed by IRAS (Sykes and Greenberg 1986). The formation of the Veritas family 8.3 Myr ago still accounts for ∼25% of the Zodiacal thermal emission today (Dermott et al 2002). A major peak of dust production in the inner Solar system is expected to have occurred at the time of the LHB ( §4), as a consequence of an increased rate of asteroidal collisions and to the collisions of numerous impactors originating in the main asteroid belt (Strom et al 2005) with the terrestrial planets.…”

Section: Inner Solar System: Asteroidal and Cometary Dustmentioning

confidence: 99%

“…The thermal emission of the Zodiacal cloud dominates the night sky between 5-500 µm and has a fractional luminosity of L dust /L Sun ∼ 10 −8 -10 −7 (Dermott et al 2002). Studied by IRAS, COBE and ISO space telescopes, it shows a featureless spectrum produced by a dominant population of low albedo (<0.08) rapidly-rotating amorphous forsterite/olivine grains that are 10-100 µm in size and are located near 1 AU.…”

Section: Inner Solar System: Asteroidal and Cometary Dustmentioning

confidence: 99%

The Kuiper Belt and Other Debris Disks

Jewitt

Moro‐Martín

Lacerda

Astrophysics in the Next Decade

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We discuss the current knowledge of the Solar system, focusing on bodies in the outer regions, on the information they provide concerning Solar system formation, and on the possible relationships that may exist between our system and the debris disks of other stars. Beyond the domains of the Terrestrial and giant planets, the comets in the Kuiper belt and the Oort cloud preserve some of our most pristine materials. The Kuiper belt, in particular, is a collisional dust source and a scientific bridge to the dusty "debris disks" observed around many nearby main-sequence stars. Study of the Solar system provides a level of detail that we cannot discern in the distant disks while observations of the disks may help to set the Solar system in proper context.

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Zodiacal Dust Bands

Cited by 44 publications

References 23 publications

EXPLORATIONS BEYOND THE SNOW LINE:SPITZER/IRS SPECTRA OF DEBRIS DISKS AROUND SOLAR-TYPE STARS

EXPLORATIONS BEYOND THE SNOW LINE:SPITZER/IRS SPECTRA OF DEBRIS DISKS AROUND SOLAR-TYPE STARS

Warm dusty discs: exploring the A star 24 μm debris population

The Kuiper Belt and Other Debris Disks

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