GG Tau: the ringworld and beyond

Dutrey, Anne; Folco, E. Di; Beck, Tracy; Guilloteau, S.

doi:10.1007/s00159-015-0091-5

Cited by 44 publications

(57 citation statements)

References 121 publications

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“…This would only comply with the observed flat velocity distribution if the 'disk' would rotate entirely in the plane of the sky, which is inconsistent with the line of sight velocity difference of the two protostars. Compared to other, tighter protostellar binary systems such as GG Tau (Dutrey et al 2014(Dutrey et al , 2016 and IRS 43 , the bridge that we observe between the components of IRAS 16293 lacks a symmetric complement to close a full circumbinary disk or torus, and its velocity structure is inconsistent with disk-like rotation. If there is any velocity gradient across the bridge, it is in the transverse direction rather than along the length of the arc.…”

Section: The Quiescent Bridgecontrasting

confidence: 79%

“…Jacobsen et al (2018 show that a dust filament model can match the observed spatial emission from high-resolution submillimeter continuum emission and C 17 O 3-2 gas line emission. Similar structures observed in other multiple protostellar systems are interpreted as fragmentation of large-scale circum-multiple envelopes (Lee et al 2017) or (Keplerian) rotating disks that have become locally gravitationally unstable (Tobin et al 2016a;Fernández-López et al 2017;Dutrey et al 2014Dutrey et al , 2016.…”

Section: Introductionsupporting

confidence: 59%

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The ALMA-PILS survey: gas dynamics in IRAS 16293−2422 and the connection between its two protostars

Wiel

Jacobsen

Jørgensen

et al. 2019

A&A

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Context. The majority of stars form in binary or higher order systems. The evolution of each protostar in a multiple system may start at different times and may progress differently. The Class 0 protostellar system IRAS 16293−2422 contains two protostars, "A" and "B", separated by ∼600 au and embedded in a single, 10 4 au scale envelope. Their relative evolutionary stages have been debated. Aims. We aim to study the relation and interplay between the two protostars A and B at spatial scales of 60 au up to ∼10 3 au. Methods. We selected molecular gas line transitions of the species CO, H 2 CO, HCN, CS, SiO, and C 2 H from the ALMA-PILS spectral imaging survey (329-363 GHz) and used them as tracers of kinematics, density, and temperature in the IRAS 16293−2422 system. The angular resolution of the PILS data set allows us to study these quantities at a resolution of 0.5 (60 au at the distance of the source).Results. Line-of-sight velocity maps of both optically thick and optically thin molecular lines reveal: (i) new manifestations of previously known outflows emanating from protostar A; (ii) a kinematically quiescent bridge of dust and gas spanning between the two protostars, with an inferred density between 4×10 4 cm −3 and ∼3×10 7 cm −3 ; and (iii) a separate, straight filament seemingly connected to protostar B seen only in C 2 H, with a flat kinematic signature. Signs of various outflows, all emanating from source A, are evidence of high-density and warmer gas; none of them coincide spatially and kinematically with the bridge. Conclusions. We hypothesize that the bridge arc is a remnant of filamentary substructure in the protostellar envelope material from which protostellar sources A and B have formed. One particular morphological structure appears to be due to outflowing gas impacting the quiescent bridge material. The continuing lack of clear outflow signatures unambiguously associated to protostar B and the vertically extended shape derived for its disk-like structure lead us to conclude that source B may be in an earlier evolutionary stage than source A.

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Section: The Quiescent Bridgecontrasting

confidence: 79%

Section: Introductionsupporting

confidence: 59%

The ALMA-PILS survey: gas dynamics in IRAS 16293−2422 and the connection between its two protostars

Wiel

Jacobsen

Jørgensen

et al. 2019

A&A

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“…Direct accretion onto the stars in the binary is only expected for spectroscopic binaries with separations of a fraction of an au. In wider systems, inner circumprimary and circumsecondary disks are expected to be fed and maintained by the streams (Günther & Kley 2002;Dutrey et al 2016). Observations of GG Tau (Dutrey et al 1994(Dutrey et al , 2014, with a projected separation of ∼ 35 au, UY Aur (Close et al 1998;Duvert et al 1998;Tang et al 2014), ∼ 125 au, and L1551 (Takakuwa et al 2014), ∼ 70 au, fit such a scenario.…”

Section: Mass J16075796-2040087: An Accreting Circumbinary Diskmentioning

confidence: 99%

The Effect of Binarity on Circumstellar Disk Evolution

Barenfeld

Carpenter

Sargent

et al. 2019

ApJ

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We present new results on how the presence of stellar companions affects disk evolution based on a study of the 5-11 Myr old Upper Scorpius OB Association. Of the 50 G0-M3 Upper Sco members with disks in our sample, only seven host a stellar companion within 2 and brighter than K = 15, compared to 35 of 75 members without disks. This matches a trend seen in the 1-2 Myr old Taurus region, where systems with a stellar companion within 40 au have a lower fraction of infrared-identified disks than those without such companions, indicating shorter disk lifetimes in close multiple systems. However, the fractions of disk systems with a stellar companion within 40 au match in Upper Sco and Taurus. Additionally, we see no difference in the millimeter brightnesses of disks in Upper Sco systems with and without companions, in contrast to Taurus where systems with a companion within 300 au are significantly fainter than wider and single systems. These results suggest that the effects of stellar companions on disk lifetimes occur within the first 1-2 Myr of disk evolution, after which companions play little further role. By contrast, disks around single stars lose the millimeter-sized dust grains in their outer regions between ages of 1-2 Myr and 5-11 Myr. The end result of small dust disk sizes and faint millimeter luminosities is the same whether the disk has been truncated by a companion or has evolved through internal processes.

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“…Other aspects of the expected circumbinary disk structure have been seen in wider binaries where features can be more readily spatially resolved, such as circumbinary rings and streams (e.g., GG Tau; Dutrey et al 2016). In close binaries such as DQ Tau, these regions of the system can be probed with multi-epoch infrared observations, particularly at wavelengths ≥ 2µm where warm dust emission becomes significant.…”

Section: Introductionmentioning

confidence: 99%

The Inner Disk and Accretion Flow of the Close Binary DQ Tau

Muzerolle

Flaherty

Balog

et al. 2019

ApJ

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We present multi-epoch optical and near-infrared (NIR) photometry and spectroscopy of the spectroscopic binary T Tauri star DQ Tau. The photometric monitoring, obtained using SMARTS ANDICAM, recovers the previously-seen correlation between optical flux and the 15.8-day binary orbital period, with blue flux peaks occurring close to most observed periastron passages. For the first time, we find an even more consistent correlation between orbital period and NIR brightness and color. The onset of pulse events in the NIR on average precedes those in the optical by a few days, with the rise usually starting near apastron orbital phase. We further obtained five epochs of spectroscopy using IRTF SpeX, with a wavelength range of 0.8 to 5 microns, and derived spectra of the infrared excess emission. The shape and strength of the excess varies with time, with cooler and weaker characteristic dust emission (T ∼ 1100 − 1300 K) over most of the binary orbit, and stronger/warmer dust emission (T ∼ 1600 K, indicative of dust sublimation) just before periastron passage. We suggest our results are broadly consistent with predictions of simulations of disk structure and accretion flows around close binaries, with the varying dust emission possibly tracing the evolution of accretion streams falling inwards through a circumbinary disk cavity and feeding the accretion pulses traced by the optical photometry and NIR emission lines. However, our results also show more complicated behavior that is not fully explained by this simple picture, and will require further observations and modeling to fully interpret.

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GG Tau: the ringworld and beyond

Cited by 44 publications

References 121 publications

The ALMA-PILS survey: gas dynamics in IRAS 16293−2422 and the connection between its two protostars

The ALMA-PILS survey: gas dynamics in IRAS 16293−2422 and the connection between its two protostars

The Effect of Binarity on Circumstellar Disk Evolution

The Inner Disk and Accretion Flow of the Close Binary DQ Tau

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