Binarity as a Key Factor in Protoplanetary Disk Evolution:
                    <i>Spitzer</i>
                    Disk Census of the η Chamaeleontis Cluster

Bouwman, J.; Lawson, W. A.; Dominik, C.; Feigelson, E. D.; Henning, Th.; Tielens, A. G. G. M.; Waters, L. B. F. M.

doi:10.1086/510365

Cited by 104 publications

(122 citation statements)

References 23 publications

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“…Bouwman et al (2006) suggest that close binaries may lose their discs significantly faster based on mid-infrared observations, meaning that most disc bearing CTTS are not generally found in close binaries. Daemgen et al (2013) resolved the components of 19 T Tauri binaries in Chameleon I.…”

Section: Bias Due To Unresolved Binariesmentioning

confidence: 96%

Classical T Tauri stars with VPHAS+ – I. H α andu-band accretion rates in the Lagoon Nebula M8

Kalari

Drew

Barentsen

et al. 2015

Mon. Not. R. Astron. Soc.

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We estimate the accretion rates of 235 Classical T Tauri star (CTTS) candidates in the Lagoon Nebula using ugriHα photometry from the VPHAS+ survey. Our sample consists of stars displaying Hα-excess, the intensity of which is used to derive accretion rates. For a subset of 87 stars, the intensity of the u-band excess is also used to estimate accretion rates. We find the mean variation in accretion rates measured using Hα and u-band intensities to be ∼ 0.17 dex, agreeing with previous estimates (0.04-0.4 dex) but for a much larger sample. The spatial distribution of CTTS align with the location of protostars and molecular gas suggesting that they retain an imprint of the natal gas fragmentation process. Strong accretors are concentrated spatially, while weak accretors are more distributed. Our results do not support the sequential star forming processes suggested in the literature.

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Section: Bias Due To Unresolved Binariesmentioning

confidence: 96%

Classical T Tauri stars with VPHAS+ – I. H α andu-band accretion rates in the Lagoon Nebula M8

Kalari

Drew

Barentsen

et al. 2015

Mon. Not. R. Astron. Soc.

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“…This is suggestive of a bimodal mechanism responsible for disk dissipation in these regions. Very early in the evolution of the associations, 30-40% of the disks may have been dissipated quickly by some efficient mechanism, for example, interaction with binary companions in close systems (Bouwman et al 2006;Kraus et al 2012). After the fast disk-dissipation phase, the remaining disks would evolve slowly via other mechanisms, e.g., viscous evolution, planet formation, or photoevaporation.…”

Section: The Disk and Accretor Frequencies In Chamentioning

confidence: 99%

“…Nearby pre-main sequence (PMS) associations at ∼50-300 pc are well suited for detailed investigations of young stars and their disks, since their members can be observed with high signal-to-noise ratio (S/N) throughout the electromagnetic spectrum. Several PMS associations have been studied with the Spitzer Space Telescope, e.g., MBM 12, Cha, and η Cha (Meeus et al 2009;Megeath et al 2005;Bouwman et al 2006;Sicilia-Aguilar et al 2009) using the infrared array camera (IRAC, Fazio et al 2004), the multiband imaging photometer for Spitzer (MIPS, Rieke et al 2004), and the infrared spectrograph (IRS, Houck et al 2004). The Spitzer data allow characterization of the disks around low-mass Based on observations performed at ESO's La Silla-Paranal observatory under programme 076.C-0470.…”

Section: Introductionmentioning

confidence: 99%

Young stars inϵChamaleontis and their disks: disk evolution in sparse associations

Fang

Boekel

Bouwman

et al. 2012

A&A

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Context. The nearby young stellar association Cha has an estimated age of 3-5 Myr, making it an ideal laboratory to study the disk dissipation process and provide empirical constraints on the timescale of planet formation. Aims. We wish to complement existing optical and near-infrared data of the Cha association, which provide the stellar properties of its members, with mid-infrared data that probe the presence, geometry, and mineralogical composition of protoplanetary disks around individual stars. Methods. We combine the available literature data with our Spitzer/IRS spectroscopy and VLT/VISIR imaging data. We use proper motions to refine the membership of Cha. Masses and ages of individual stars are estimated by fitting model atmospheres to the optical and near-infrared photometry, followed by placement in the Hertzsprung-Russell diagram. The Spitzer/IRS spectra are analyzed using the two-layer temperature distribution spectral decomposition method. Results. Two stars previously identified as members, CXOU J120152.8 and 2MASS J12074597, have proper motions that are very different from those of the other stars. But other observations suggest that the two stars are still young and thus might still be related to Cha. HD 104237C is the lowest mass member of Cha with an estimated mass of ∼13-15 Jupiter masses. The very low mass stars USNO-B120144.7 and 2MASS J12005517 show globally depleted spectral energy distributions, pointing at strong dust settling. 2MASS J12014343 may have a disk with a very specific inclination, where the central star is effectively screened by the cold outer parts of a flared disk, but the 10 μm radiation of the warm inner disk can still reach us. We find that the disks in sparse stellar associations are dissipated more slowly than those in denser (cluster) environments. We detect C 2 H 2 rovibrational band around 13.7 μm on the IRS spectrum of USNO-B120144.7. We find strong signatures of grain growth and crystallization in all Cha members with 10 μm features detected in their IRS spectra. We combine the dust properties derived in the Cha sample with those found using identical or similar methods in the MBM 12, Coronet, η Cha associations, and in the cores-to-disks legacy program. We find that disks around low-mass young stars show a negative radial gradient in the mass-averaged grain size and mass fraction of crystalline silicates. A positive correlation exists between the mass-averaged grain sizes of amorphous silicates and the accretion rates if the latter is above ∼10 −9 M yr −1 , possibly indicating that those disks are sufficiently turbulent to prevent grains of several microns in size to sink into the disk interior.

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“…Haisch et al 2001;Bouwman et al 2006;Jayawardhana et al 2006;Sicilia-Aguilar et al 2006;Fedele et al 2010). At this age, stars lose their inner dusty disk and accretion stops.…”

Section: Stellar Spotsmentioning

confidence: 99%

HD 135344B: a young star has reached its rotational limit

Müller

Ancker

Launhardt

et al. 2011

A&A

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Aims. We search for periodic variations in the radial velocity of the young Herbig star HD 135344B to determine a rotation period. Methods. We analyze 44 high-resolution optical spectra taken over a time period of 151 days. The spectra were acquired with FEROS at the 2.2 m MPG/ESO telescope in La Silla. The stellar parameters of HD 135344B are determined by fitting synthetic spectra to the stellar spectrum. To obtain radial velocity measurements, the stellar spectra are cross-correlated with a theoretical template computed from determined stellar parameters. Results. We report the first direct measurement of the rotation period of a Herbig star from radial velocity measurements. The rotation period is found to be 0.16 d (3.9 h), which makes HD 135344B a rapid rotator at or close to its break-up velocity. The rapid rotation could explain some of the properties of the circumstellar environment of HD 135344B such as an inner disk with properties (composition, inclination) that differ significantly from the outer disk.

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Binarity as a Key Factor in Protoplanetary Disk Evolution: Spitzer Disk Census of the η Chamaeleontis Cluster

Cited by 104 publications

References 23 publications

Classical T Tauri stars with VPHAS+ – I. H α andu-band accretion rates in the Lagoon Nebula M8

Classical T Tauri stars with VPHAS+ – I. H α andu-band accretion rates in the Lagoon Nebula M8

Young stars inϵChamaleontis and their disks: disk evolution in sparse associations

HD 135344B: a young star has reached its rotational limit

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