An ALMA survey for disks orbiting low-mass stars in the TW Hya Association

Rodríguez, David; Plas, G. van der; Kastner, Joel H.; Schneider, Adam C.; Faherty, Jacqueline K.; Mardones, Diego; Mohanty, Subhanjoy; Principe, David A.

doi:10.1051/0004-6361/201527031

Cited by 23 publications

(28 citation statements)

References 42 publications

(69 reference statements)

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“…Furthermore, most of the newly discovered TWA candidates that are of late-M and L-type also display evidence for disks (Rodriguez et al 2015). The extant data for the TWA hence suggest that disk survival times may be longer for ultra-low mass stars and brown dwarfs than for higher-mass (early-type) M stars-a result that would be consistent with studies of the Upper Sco region (age ∼10 Myr; Scholz et al 2007;Luhman & Mamajek 2012, and references therein).…”

Section: Discussionsupporting

confidence: 75%

“…However, only TWA 30B was detected as a submillimeter continuum source, and none of the three were detected as CO sources, in the Rodriguez et al (2015) ALMA survey of ultralow-mass members and candidate members of the TWA. The CO nondetections imply the gas disks orbiting these three stars have very low masses and/or small radii (0.1 Earth masses and/or 10 au, respectively; Rodriguez et al 2015).…”

Section: Presence or Absence Of Circumstellar Disksmentioning

confidence: 93%

“…Due to their small radial extent and low masses, the gaseous constituents of these disks are exceedingly difficult to detect in (sub)millimeter-wave molecular line emission. Indeed, as noted in Section 2.2, gas has been detected in the disks orbiting TWA 30A and 30B in the form of optical forbidden-line emission from disk winds and jets (Looper et al 2010a(Looper et al , 2010b as well as X-ray absorption by the (nearly edge-on) TWA 30A disk itself (Principe et al 2016); however, a sensitive search for CO in these same disks with ALMA yielded negative results (Rodriguez et al 2015).…”

Section: Implications For Disk Dispersal Via Photoevaporationmentioning

confidence: 99%

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M Stars in the Tw Hya Association: Stellar X-Rays and Disk Dissipation

Kastner¹,

Principe²,

Punzi³

et al. 2016

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To investigate the potential connection between the intense X-ray emission from young low-mass stars and the lifetimes of their circumstellar planet-forming disks, we have compiled the X-ray luminosities (L X ) of M stars in the ∼8 Myr old TW Hya Association (TWA) for which X-ray data are presently available. Our investigation includes analysis of archival Chandra data for the TWA binary systems TWA 8, 9, and 13. Although our study suffers from poor statistics for stars later than M3, we find a trend of decreasing L L X bol with decreasing T eff for TWA M stars, wherein the earliest-typeand then ( ) L L log X bol decreases, and its distribution broadens, for types M4 and later. The fraction of TWA stars that display evidence for residual primordial disk material also sharply increases in this same (mid-M) spectral type regime. This apparent anticorrelation between the relative X-ray luminosities of low-mass TWA stars and the longevities of their circumstellar disks suggests that primordial disks orbiting early-type M stars in the TWA have dispersed rapidly as a consequence of their persistent large X-ray fluxes. Conversely, the disks orbiting the very lowest-mass pre-MS stars and pre-MS brown dwarfs in the Association may have survived because their X-ray luminosities and, hence, disk photoevaporation rates are very low to begin with, and then further decline relatively early in their pre-MS evolution.

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Section: Discussionsupporting

confidence: 75%

Section: Presence or Absence Of Circumstellar Disksmentioning

confidence: 93%

Section: Implications For Disk Dispersal Via Photoevaporationmentioning

confidence: 99%

See 1 more Smart Citation

M Stars in the Tw Hya Association: Stellar X-Rays and Disk Dissipation

Kastner¹,

Principe²,

Punzi³

et al. 2016

Self Cite

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“…CO line emission has been previously found to be fainter than expected from the dust emission, assuming the canonical ISM gas-to-dust and [CO]/[H 2 ] ratios (e.g., Dutrey et al 2003;Chapillon et al 2008;Rodriguez et al 2015;Pericaud et al 2016). This conclusion, from small and biased samples, was recently strengthened in a large and unbiased sample of disks in the Lupus star-forming region (Ansdell et al 2016;Miotello et al 2017) and is confirmed here for a complete survey of disks from the young (2-3Myr) ChaI star-forming region.…”

Section: Co Depletion and Implications For Planet Formationmentioning

confidence: 99%

An ALMA Survey of CO Isotopologue Emission from Protoplanetary Disks in Chamaeleon I

Long

Herczeg

Pascucci

et al. 2017

ApJ

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137

142

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The mass of a protoplanetary disk limits the formation and future growth of any planet. Masses of protoplanetary disks are usually calculated from measurements of the dust continuum emission by assuming an interstellar gas-todust ratio. To investigate the utility of CO as an alternate probe of disk mass, we use ALMA to survey 13 CO and C 18 O J=3-2 line emission from a sample of 93 protoplanetary disks around stars and brown dwarfs with masses from M 0.03 to 2  in the nearby Chamaeleon I star-forming region. We detect 13 CO emission from 17 sources and C 18 O from only one source. Gas masses for disks are then estimated by comparing the CO line luminosities to results from published disk models that include CO freeze-out and isotope-selective photodissociation. Under the assumption of a typical interstellar medium CO-to-H 2 ratio of 10 −4 , the resulting gas masses are implausibly low, with an average gas mass of ∼0.05 M Jup as inferred from the average flux of stacked 13 CO lines. The low gas masses and gas-to-dust ratios for Cha I disks are both consistent with similar results from disks in the Lupus starforming region. The faint CO line emission may instead be explained if disks have much higher gas masses, but freeze-out of CO or complex C-bearing molecules is underestimated in disk models. The conversion of CO flux to CO gas mass also suffers from uncertainties in disk structures, which could affect gas temperatures. CO emission lines will only be a good tracer of the disk mass when models for C and CO depletion are confirmed to be accurate.

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“…This dust mass could be associated with the disk of UX Tauri C. A similar upper limit can be considered for the component UX Tauri B. Molecular disks have been detected toward a handful of low mass or substellar objects. Some examples are IC 348-SMM2E (Palau et al 2014), TWA 34 (Rodriguez et al 2015), Rho Oph 102 (Ricci et al 2012) and 2MASS J04442713+2512164 (Ricci et al 2014). However, none of these disks seem to be associated with a multiple system as UX Tauri.…”

Section: Dust and Gas Massmentioning

confidence: 99%

Tidal Interaction between the UX Tauri A/C Disk System Revealed by ALMA

Zapata¹,

Rodrı́guez

Fernández-López

et al. 2020

ApJ

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We present sensitive and high angular resolution (∼0.2-0.3 ) (sub)millimeter (230 and 345 GHz) continuum and CO(2−1)/CO(3−2) line archive observations of the disk star system in UX Tauri carried out with ALMA (The Atacama Large Millimeter/Submillimeter Array). These observations reveal the gas and dusty disk surrounding the young star UX Tauri A with a large signal-to-noise ratio (>400 in the continuum and >50 in the line), and for the first time is detected the molecular gas emission associated with the disk of UX Tauri C (with a size for the disk of <56 au). No (sub)millimeter continuum emission is detected at 5σ-level (0.2 mJy at 0.85 mm) associated with UX Tauri C. For the component UX Tauri C, we estimate a dust disk mass of ≤ 0.05 M ⊕ . Additionally, we report a strong tidal disk interaction between both disks UX Tauri A/C, separated 360 au in projected distance. The CO line observations reveal marked spiral arms in the disk of UX Tauri A and an extended redshifted stream of gas associated with the UX Tauri C disk. No spiral arms are observed in the dust continuum emission of UX Tauri A. Assuming a Keplerian rotation we estimate the enclosed masses (disk+star) from their radial velocities in 1.4 ± 0.6 M for UX Tauri A, and 70 ± 30 / sin i Jupiter masses for UX Tauri C (the latter coincides with the mass upper limit value for a brown dwarf). The observational evidence presented here lead us to propose that UX Tauri C is having a close approach of a possible wide, evolving and eccentric orbit around the disk of UX Tauri A causing the formation of spiral arms and the stream of molecular gas falling towards UX Tauri C.

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An ALMA survey for disks orbiting low-mass stars in the TW Hya Association

Cited by 23 publications

References 42 publications

M Stars in the Tw Hya Association: Stellar X-Rays and Disk Dissipation

M Stars in the Tw Hya Association: Stellar X-Rays and Disk Dissipation

An ALMA Survey of CO Isotopologue Emission from Protoplanetary Disks in Chamaeleon I

Tidal Interaction between the UX Tauri A/C Disk System Revealed by ALMA

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