A Sub-AU Outwardly Truncated Accretion Disk around a Classical T Tauri Star

McClure, Melissa; Forrest, W. J.; Sargent, B.; Watson, D. M.; Furlan, Elise; Manoj, P.; Luhman, K. L.; Calvet, Nuria; Espaillat, Catherine; D’Alessio, Paola; Hartmann, L.; Tayrien, C.; Harrold, Samuel T.

doi:10.1086/591666

Cited by 15 publications

(15 citation statements)

References 36 publications

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“…Some theoretical studies already pointed to the possible existence of a relatively large population of very small disks (McClure et al 2008, Piétu et al 2014, Kraus et al 2015, Furlan et al 2016. However, none of these putative dwarf disks has been angularly resolved.…”

Section: Discussionmentioning

confidence: 99%

“…Typical transitional disks imaged so far have radii of 50-100 au and masses of 10-100 M J , with central cavities of 15-70 au in radius (Andrews et al 2011, Espaillat et al 2014, Andrews 2015. Nevertheless, some results, based on the spectral energy distribution (SED) modeling, suggest that significantly smaller disks should exist (McClure et al 2008, Piétu et al 2014), but direct imaging has not been possible yet.…”

Section: Introductionmentioning

confidence: 98%

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A Dwarf Transitional Protoplanetary Disk Around Xz Tau B

Osorio

Macías

Anglada

et al. 2016

ApJL

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We report the discovery of a dwarf protoplanetary disk around the star XZ Tau B that shows all the features of a classical transitional disk but on a much smaller scale. The disk has been imaged with the Atacama Large Millimeter/Submillimeter Array (ALMA), revealing that its dust emission has a quite small radius of ∼3.4 au and presents a central cavity of ∼1.3 au in radius that we attribute to clearing by a compact system of orbiting (proto)planets. Given the very small radii involved, evolution is expected to be much faster in this disk (observable changes in a few months) than in classical disks (observable changes requiring decades) and easy to monitor with observations in the near future. From our modeling we estimate that the mass of the disk is large enough to form a compact planetary system.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 98%

A Dwarf Transitional Protoplanetary Disk Around Xz Tau B

Osorio

Macías

Anglada

et al. 2016

ApJL

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“…In the millimeter, we are more sensitive to the 18 The SED of FM 581 resembles that of the 5-10 AU binary SR 20 (McClure et al 2008). SR 20's disk is outwardly truncated at 0.4 AU, too far to be attributable to the known companion, and so this truncation would have to be due to an unseen companion at ∼1-2 AU (McClure et al 2008). Likewise, it seems that the most viable mechanism to truncate the disk of FM 581 to such small radii would also be a companion.…”

Section: Model Degeneracies and Millimeter Constraintsmentioning

confidence: 98%

On the Transitional Disk Class: Linking Observations of T Tauri Stars and Physical Disk Models

Espaillat

Ingleby

Hernández³

et al. 2012

ApJ

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Two decades ago "transitional disks" described spectral energy distributions (SEDs) of T Tauri stars with small near-IR excesses, but significant mid-and far-IR excesses. Many inferred this indicated dust-free holes in disks, possibly cleared by planets. Recently, this term has been applied disparately to objects whose Spitzer SEDs diverge from the expectations for a typical full disk. Here we use irradiated accretion disk models to fit the SEDs of 15 such disks in NGC 2068 and IC 348. One group has a "dip" in infrared emission while the others' continuum emission decreases steadily at all wavelengths. We find that the former have an inner disk hole or gap at intermediate radii in the disk and we call these objects "transitional" and "pre-transitional" disks, respectively. For the latter group, we can fit these SEDs with full disk models and find that millimeter data are necessary to break the degeneracy between dust settling and disk mass. We suggest the term "transitional" only be applied to objects that display evidence for a radical change in the disk's radial structure. Using this definition, we find that transitional and pre-transitional disks tend to have lower mass accretion rates than full disks and that transitional disks have lower accretion rates than pre-transitional disks. These reduced accretion rates onto the star could be linked to forming planets. Future observations of transitional and pre-transitional disks will allow us to better quantify the signatures of planet formation in young disks.

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“…For orbital separations of ∼200 AU, companions truncate the disk from outside (for typical disk sizes of ∼100 AU); for even smaller orbital separations ( a few tens of AU) the disk could be truncated from inside as in the case of CoKu Tau/4 (Ireland & Kraus 2008). An outwardly truncated disk is likely to show a steeper mid-IR continuum slope, i.e., n 13-31 less than that for a flat disk (McClure et al 2008). Similarly, disks truncated from inside will have significantly steeper n 6-13 continuum index.…”

Section: Multiplicity and Disk Structurementioning

confidence: 99%

SPITZER INFRARED SPECTROGRAPH SURVEY OF YOUNG STARS IN THE CHAMAELEON I STAR-FORMING REGION

Manoj

Kim

Furlan

et al. 2011

ApJS

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We present 5-36 μm mid-infrared spectra of 82 young stars in the ∼2 Myr old Chamaeleon I star-forming region, obtained with the Spitzer Infrared Spectrograph (IRS). We have classified these objects into various evolutionary classes based on their spectral energy distributions and the spectral features seen in the IRS spectra. We have analyzed the mid-IR spectra of Class II objects in Chamaeleon I in detail, in order to study the vertical and radial structure of the protoplanetary disks surrounding these stars. We find evidence for substantial dust settling in most protoplanetary disks in Chamaeleon I. We have identified several disks with altered radial structures in Chamaeleon I, among them transitional disk candidates which have holes or gaps in their disks. Analysis of the silicate emission features in the IRS spectra of Class II objects in Cha I shows that the dust grains in these disks have undergone significant processing (grain growth and crystallization). However, disks with radial holes/gaps appear to have relatively unprocessed grains. We further find the crystalline dust content in the inner ( 1-2 AU) and the intermediate ( 10 AU) regions of the protoplanetary disks to be tightly correlated. We also investigate the effects of accretion and stellar multiplicity on the disk structure and dust properties. Finally, we compare the observed properties of protoplanetary disks in Cha I with those in slightly younger Taurus and Ophiuchus regions and discuss the effects of disk evolution in the first 1-2 Myr.

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A Sub-AU Outwardly Truncated Accretion Disk around a Classical T Tauri Star

Cited by 15 publications

References 36 publications

A Dwarf Transitional Protoplanetary Disk Around Xz Tau B

A Dwarf Transitional Protoplanetary Disk Around Xz Tau B

On the Transitional Disk Class: Linking Observations of T Tauri Stars and Physical Disk Models

SPITZER INFRARED SPECTROGRAPH SURVEY OF YOUNG STARS IN THE CHAMAELEON I STAR-FORMING REGION

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