The effect of stellar multiplicity on protoplanetary discs: a near-infrared survey of the Lupus star-forming region

Zurlo, A.; Cieza, Lucas A.; Ansdell, Megan; Christiaens, Valentin; Pérez, Sebastián; Lovell, Joshua B.; Mesa, D.; Williams, Jonathan P.; González-Ruilova, Camilo; Carraro, R.; Ruíz-Rodríguez, Dary; Wyatt, M. C.

doi:10.1093/mnras/staa3674

Cited by 33 publications

(34 citation statements)

References 42 publications

(69 reference statements)

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“…7, the larger the truncation radius, the brighter and larger the binary discs are. Such an evidence is in qualitative agreement with the observational results of Harris et al (2012); Cox et al (2017); Akeson et al (2019); Zurlo et al (2020) and Zurlo et al (2021), who found larger fluxes in wider binaries (recall Fig. 1), as well as those of Manara et al (2019) and Zurlo et al (2020Zurlo et al ( , 2021 who find smaller discs in multiple systems than around isolated stars.…”

Section: Flux-radius Correlation In Binary Disc Modelssupporting

confidence: 92%

“…Such an evidence is in qualitative agreement with the observational results of Harris et al (2012); Cox et al (2017); Akeson et al (2019); Zurlo et al (2020) and Zurlo et al (2021), who found larger fluxes in wider binaries (recall Fig. 1), as well as those of Manara et al (2019) and Zurlo et al (2020Zurlo et al ( , 2021 who find smaller discs in multiple systems than around isolated stars. When 𝑅 trunc 100 au the model fluxes and radii are tightly correlated, behaving as in single-star discs 9 and following the quadratic relation in Tripathi et al (2017) at almost every time.…”

Section: Flux-radius Correlation In Binary Disc Modelssupporting

confidence: 92%

“…They found that the flux of each stellar pair 1 , the sum of the fluxes of the two pair components, increases with its separation in discrete jumps (roughly by a factor of five for binaries wider than 𝑎 p = 30 au and 300 au). We collect archival data from multiple stellar disc surveys in Taurus (Harris et al 2012;Akeson & Jensen 2014;Akeson et al 2019;Manara et al 2019), 𝜌 Ophiuchus (Cox et al 2017;Cieza et al 2019;Williams et al 2019;Zurlo et al 2020) and Lupus (Ansdell et al 2018;Zurlo et al 2021) with the aim of discussing if Harris et al (2012) trends are still valid in a larger sample, with discs from different star-forming regions of the same age.…”

Section: A Logbook Of Binary Disc Observationsmentioning

confidence: 99%

“…In Flux-separation correlation in pairs Survey: Manara et al 2019Akeson et al 2019Akeson&Jensen 2014Harris et al 2012Ansdell et al 2018Zurlo et al 2021Cieza et al 2019William et al 2019Zurlo et al 2020Cox et al 2017 Figure 1. The 0.85 mm flux in binary pairs, 𝐹 pair , as a function of their projected separation, 𝑎 p , for multiple stellar discs in Taurus, 𝜌 Ophiuchus and Lupus.…”

Section: A Logbook Of Binary Disc Observationsmentioning

confidence: 99%

“…In the young (1 − 3 Myr old) Taurus-Auriga, 𝜌 Ophiuchus and Lupus star-forming regions, Harris et al (2012), using SMA data, as well as Cox et al (2017); Akeson et al (2019); Zurlo et al (2020) and Zurlo et al (2021), using ALMA data, showed that binary discs are significantly fainter in the continuum than the single-star ones. Moreover, Harris et al (2012); Akeson et al (2019); Zurlo et al (2020) and Zurlo et al (2021) showed that binary disc fluxes increase with the stellar separation and that discs in wide binaries are almost as bright as the single-star ones. On the contrary, in the older (5 − 11 Myr old) Upper Scorpius OB-association, Barenfeld et al (2019) found no statistically relevant differences between binary and singlestar disc brightness distribution.…”

Section: Introductionmentioning

confidence: 99%

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On dust evolution in planet-forming discs in binary systems – II. Comparison with Taurus and ρ Ophiuchus (sub-)millimetre observations: discs in binaries have small dust sizes

Zagaria

Rosotti

Lodato

2021

Monthly Notices of the Royal Astronomical Society

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The recently discovered exoplanets in binary or higher-order multiple stellar systems sparked a new interest in the study of proto-planetary discs in stellar aggregations. Here we focus on disc solids, as they make up the reservoir out of which exoplanets are assembled and dominate (sub-)millimetre disc observations. These observations suggest that discs in binary systems are fainter and smaller than in isolated systems. In addition, disc dust sizes are consistent with tidal truncation only if they orbit very eccentric binaries. In a previous study we showed that the presence of a stellar companion hastens the radial migration of solids, shortening disc lifetime and challenging planet formation. In this paper we confront our theoretical and numerical results with observations: disc dust fluxes and sizes from our models are computed at ALMA wavelengths and compared with Taurus and ρ Ophiuchus data. A general agreement between theory and observations is found. In particular, we show that the dust disc sizes are generally smaller than the binary truncation radius due to the combined effect of grain growth and radial drift: therefore, small disc sizes do not require implausibly high eccentricities to be explained. Furthermore, the observed binary discs are compatible within 1σ with a quadratic flux-radius correlation similar to that found for single-star discs and show a close match with the models. However, the observational sample of resolved binary discs is still small and additional data are required to draw more robust conclusions on the flux-radius correlation and how it depends on the binary properties.

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Section: Flux-radius Correlation In Binary Disc Modelssupporting

confidence: 92%

Section: Flux-radius Correlation In Binary Disc Modelssupporting

confidence: 92%

Section: A Logbook Of Binary Disc Observationsmentioning

confidence: 99%

Section: A Logbook Of Binary Disc Observationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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On dust evolution in planet-forming discs in binary systems – II. Comparison with Taurus and ρ Ophiuchus (sub-)millimetre observations: discs in binaries have small dust sizes

Zagaria

Rosotti

Lodato

2021

Monthly Notices of the Royal Astronomical Society

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New binaries from the SHINE survey

Bonavita¹,

Gratton²,

Desidera³

et al. 2022

A&A

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We present the multiple stellar systems observed within the SpHere INfrared survey for Exoplanet (SHINE). SHINE searched for sub-stellar companions to young stars using high contrast imaging. Although stars with known stellar companions within the SPHERE field of view (< 5.5 arcsec) were removed from the original target list, we detected additional stellar companions to 78 of the 463 SHINE targets observed so far. Twenty-seven per cent of the systems have three or more components. Given the heterogeneity of the sample in terms of observing conditions and strategy, tailored routines were used for data reduction and analysis, some of which were specifically designed for these datasets. We then combined SPHERE data with literature and archival data, TESS light curves, and Gaia parallaxes and proper motions for an accurate characterisation of the systems. Combining all data, we were able to constrain the orbits of 25 systems. We carefully assessed the completeness of our sample for separations between 50–500 mas (corresponding to periods of a few years to a few decades), taking into account the initial selection biases and recovering part of the systems excluded from the original list due to their multiplicity. This allowed us to compare the binary frequency for our sample with previous studies and highlight interesting trends in the mass ratio and period distribution. We also found that, when such an estimate was possible, the values of the masses derived from dynamical arguments were in good agreement with the model predictions. Stellar and orbital spins appear fairly well aligned for the 12 stars that have enough data, which favours a disk fragmentation origin. Our results highlight the importance of combining different techniques when tackling complex problems such as the formation of binaries and show how large samples can be useful for more than one purpose.

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Observational constraints on gas disc sizes in the protoplanetary discs of multiple systems in the Taurus region

Rota

Manara

Miotello

et al. 2022

A&A

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The formation of multiple stellar systems is a natural by-product of the star-formation process, and its impact on the properties of protoplanetary discs and on the formation of planets is not yet fully understood. To date, no detailed uniform study of the gas emission from a sample of protoplanetary discs around multiple stellar systems has been performed. Here we analyse new ALMA observations of the molecular CO gas emission at a ~21 au resolution, specifically targeting discs in eight multiple stellar systems in the Taurus star-forming regions. 12CO gas emission is detected around all primaries and in seven companions. With these data, we estimate the inclination and the position angle (PA) for all primary discs and for five secondary or tertiary discs, and measure the gas disc radii of these objects with a cumulative flux technique on the spatially resolved zeroth moment images. When considering the radius, including 95% of the flux as a metric, the estimated size of the gas disc in multiple stellar systems is found to be on average ~4.2 times larger than the size of the dust disc. This ratio is higher than what was recently found in a population of more isolated and single systems. On the contrary, when considering the radius including 68% of the flux, no difference between multiple and single discs is found in the distribution of ratios. This discrepancy is due to the sharp truncation of the outer dusty disc observed in multiple stellar systems. The measured sizes of gas discs are consistent with tidal truncation models in multiple stellar systems assuming eccentricities of ~0.15–0.5, as expected in typical binary systems.

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The effect of stellar multiplicity on protoplanetary discs: a near-infrared survey of the Lupus star-forming region

Cited by 33 publications

References 42 publications

On dust evolution in planet-forming discs in binary systems – II. Comparison with Taurus and ρ Ophiuchus (sub-)millimetre observations: discs in binaries have small dust sizes

On dust evolution in planet-forming discs in binary systems – II. Comparison with Taurus and ρ Ophiuchus (sub-)millimetre observations: discs in binaries have small dust sizes

New binaries from the SHINE survey

Observational constraints on gas disc sizes in the protoplanetary discs of multiple systems in the Taurus region

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