期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 507, 期 2, 页码 2531-2549出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stab2024
关键词
accretion; accretion discs; opacity; planets and satellites: formation; protoplanetary discs; binaries: general; circumstellar matter; submillimetre: planetary systems
资金
- Erasmus+ Traineeship program
- Science and Technology Facilities Council (STFC) studentship
- Cambridge European Scholarship
- Netherlands Organisation for Scientific Research (NWO) [016.Veni.192.233]
- STFC Ernest Rutherford Fellowship [ST/T003855/1]
- European Union [823823]
- IUSS
- STFC [ST/T003855/1] Funding Source: UKRI
The discovery of exoplanets in binary or multiple stellar systems has sparked a new interest in the study of protoplanetary discs in stellar aggregations. Observations show that discs in binary systems are fainter and smaller than in isolated systems, and the size of disc dust is consistent with tidal truncation. Additionally, the presence of a stellar companion accelerates the radial migration of solids and challenges planet formation.
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 rho 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 1 sigma 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.
作者
我是这篇论文的作者
点击您的名字以认领此论文并将其添加到您的个人资料中。
推荐
暂无数据