The recently discovered exoplanets in binary or higher order multiple stellar systems sparked a new interest in the study of protoplanetary 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.

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 / F. Zagaria, G.P. Rosotti, G. Lodato. - In: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY. - ISSN 0035-8711. - 507:2(2021), pp. 2531-2549. [10.1093/mnras/stab2024]

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

G.P. Rosotti;G. Lodato
Ultimo
2021

Abstract

The recently discovered exoplanets in binary or higher order multiple stellar systems sparked a new interest in the study of protoplanetary 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.
accretion, accretion discs; binaries: general; circumstellar matter; opacity; planets and satellites: formation; protoplanetary discs; submillimetre: planetary systems
Settore FIS/05 - Astronomia e Astrofisica
Dust and gas in planet forming discs (DUSTBUSTER)
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/2434/896497
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