Cometary Dust in the Debris Disks of HD 31648 and HD 163296: Two “Baby” β Pictoris Stars

Sitko, Michael L.; Grady, C. A.; Lynch, D. K.; Russell, R. W.; Hanner, M. S.

doi:10.1086/306586

Cited by 42 publications

(40 citation statements)

References 29 publications

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“…Some IDPs (interplanetary dust particles) have similar emissivity curves. This resemblance, which was first noted in β Pic, now extends to many related systems (Sitko et al, 1999).…”

Section: Hd 100546: Mineralogy Of Solids and Possible Cometary Activitysupporting

confidence: 52%

Beta Pictoris and other Solar Systems

Artymowicz

2000

From Dust to Terrestrial Planets

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Abstract. Planetary systems come in a bewildering variety of shapes and sizes. In addition to the exoplanetary systems with giant planets, found in surveys of stellar radial velocity variations, an overlapping class of dusty disk-containing solar systems exists. The disks include large quantities of meteoroids and dust, and a varying complement of gas. Their solid material represents 'replenished' dust born in the collisions/sublimation of planetesimals perturbed by planets. We present several such systems, including HR 4796A, HD 141569, HD 100546, and the prototypical replenished disk of Beta Pictoris. We discuss the composition, physical processing, and migration of dust in the disks, their evolutionary status, and the evidence of embedded planets.

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“…Some IDPs (interplanetary dust particles) have similar emissivity curves. This resemblance, which was first noted in β Pic, now extends to many related systems (Sitko et al, 1999).…”

Section: Hd 100546: Mineralogy Of Solids and Possible Cometary Activitysupporting

confidence: 52%

Beta Pictoris and other Solar Systems

Artymowicz

2000

From Dust to Terrestrial Planets

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“…Ground-based 10 and 20 µm work on samples of brighter sources (e.g. Hanner et al 1995Hanner et al , 1998Sitko et al 1999;van Boekel et al 2003;Kessler-Silacci et al 2005) and especially ISO 2-30 µm spectroscopy (e.g. Meeus et al 2001;Bouwman et al 2001) have revealed an impressive suite of solid state (and PAH) dust features.…”

Section: The Potential For Planet Formation In Young Circumstellar Disksmentioning

confidence: 99%

Observational constraints on dust disk lifetimes: Implications for planet formation

Hillenbrand

2008

A Decade of Extrasolar Planets Around Normal Stars

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Thus far our impressions regarding the evolutionary time scales for young circumstellar disks have been based on small number statistics. Over the past decade, however, in addition to precision study of individual star/disk systems, substantial observational effort has been invested in obtaining less detailed data on large numbers of objects in young star clusters. This has resulted in a plethora of information now enabling statistical studies of disk evolutionary diagnostics. Along an ordinate one can measure disk presence or strength through indicators such as ultraviolet/blue excess or spectroscopic emission lines tracing accretion, infrared excess tracing dust, or millimeter flux measuring mass. Along an abscissa one can track stellar age. While bulk trends in disk indicators versus age are evident, observational errors affecting both axes, combined with systematic errors in our understanding of stellar ages, both cloud and bias any such trends. Thus detailed understanding of the physical processes involved in disk dissipation and of the relevant time scales remains elusive. Nevertheless, a clear effect in current data that is unlikely to be altered by data analysis improvements is the dispersion in disk lifetimes. Inner accretion disks are traced by near-infrared emission. Moderating a generally declining trend in near-infared continuum excess and excess frequency with age over <1 to 8±4 Myr, is the fact that a substantial fraction of rather young (<1 Myr old) stars apparently have already lost their inner accretion disks while a significant number of rather old (8-16 Myr) stars apparently still retain inner accretion disks. The age at which evidence for inner accretion disks ceases to be apparent for the vast majority (∼90%) of stars is in the range 3-8 Myr. More distant, terrestrial zone dust is traced by mid-infrared emission where sufficient sensitivity and uniform data collection are only now being realized with data return from the Spitzer Space Telescope. Constraints on mid-disk dissipation and disk clearing trends with radius are forthcoming.

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“…The optical and UV spectroscopic data, particularly for Ha and Mg II, suggested that HD 163296 should resemble younger Herbig Ae stars such as AB Aur. Studies using IR spectroscopy have begun to probe the chemistry and mineralogy of the disk with detections of warm (r ¹ 30 AU ; van Dishoek et al 1998) and a wealth H 2 of silicate features (Sitko et al 1999 ;van den Ancker et al 2000) resembling cometary materials. In contrast to the optical spectra, the silicate data suggest that the system should resemble more evolved protoplanetary to young planetary disks such as b Pic.…”

Section: Introductionmentioning

confidence: 99%

STIS Coronagraphic Imaging of the Herbig Ae Star: HD 163296

Grady

Devine

Woodgate

et al. 2000

ApJ

128

217

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Coronagraphic imaging with the Space Telescope Imaging Spectrograph on board the Hubble Space T elescope reveals a D450 AU radius circumstellar disk around the Herbig Ae star HD 163296. A broadband (0.2È1.0 km) reÑected light image shows the disk oriented at a position angle of 140¡^5¡ and inclined to our line of sight by D60¡^5¡. The disk includes an annulus of reduced scattering at 325 AU and exhibits a Ñat trend of surface brightness in to 180È122 AU consistent with a cleared (1A .5È1A), central zone. For r º 370 AU the disk surface brightness drops as r to the approximately [3.5 power. The disk cannot be traced beyond 450 AU in our data. The disk is accompanied by a chain of nebulosities at compatible with detection of a Herbig-Haro Ñow. The HD 163296 disk most P.A.\42¡ .5^3¡ .5, closely resembles the disk of HD 141569. As in the HD 141569 system, the dynamical e †ects of a planet may be necessary to explain the structure in the outer disk.

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Cometary Dust in the Debris Disks of HD 31648 and HD 163296: Two “Baby” β Pictoris Stars

Cited by 42 publications

References 29 publications

Beta Pictoris and other Solar Systems

Beta Pictoris and other Solar Systems

Observational constraints on dust disk lifetimes: Implications for planet formation

STIS Coronagraphic Imaging of the Herbig Ae Star: HD 163296

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