학술논문
Mapping of shadows cast on a protoplanetary disk by a close binary system
Document Type
Working Paper
Author
D'Orazi, V.; Gratton, R.; Desidera, S.; Avenhaus, H.; Mesa, D.; Stolker, T.; Giro, E.; Benatti, S.; Jang-Condell, H.; Rigliaco, E.; Sissa, E.; Scatolin, T.; Benisty, M.; Bhowmik, T.; Boccaletti, A.; Bonnefoy, M.; Brandner, W.; Buenzli, E.; Chauvin, G.; Daemgen, S.; Damasso, M.; Feldt, M.; Galicher, R.; Girard, J.; Janson, M.; Hagelberg, J.; Mouillet, D.; Kral, Q.; Lannier, J.; Lagrange, A. M.; Langlois, M.; Maire, A. -L.; Menard, F.; Moeller-Nilsson, O.; Perrot, C.; Peretti, S.; Rabou, P.; Ramos, J.; Rodet, L.; Roelfsema, R.; Roux, A.; Salter, G.; Schlieder, J. E.; Schmidt, T.; Szulagyi, J.; Thalmann, C.; Thebault, P.; van der Plas, G.; Vigan, A.; Zurlo, A.
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Abstract
For a comprehensive understanding of planetary formation and evolution, we need to investigate the environment in which planets form: circumstellar disks. Here we present high-contrast imaging observations of V4046 Sagittarii, a 20-Myr-old close binary known to host a circumbinary disk. We have discovered the presence of rotating shadows in the disk, caused by mutual occultations of the central binary. Shadow-like features are often observed in disks\cite{garufi,marino15}, but those found thus far have not been due to eclipsing phenomena. We have used the phase difference due to light travel time to measure the flaring of the disk and the geometrical distance of the system. We calculate a distance that is in very good agreement with the value obtained from the Gaia mission's Data Release 2 (DR2), and flaring angles of $\alpha = 6.2 \pm 0.6 $ deg and $\alpha = 8.5 \pm 1.0 $ deg for the inner and outer disk rings, respectively. Our technique opens up a path to explore other binary systems, providing an independent estimate of distance and the flaring angle, a crucial parameter for disk modelling.
Comment: Authors' version of the article published in Nature Astronomy. Final version available at https://www.nature.com/natastron/
Comment: Authors' version of the article published in Nature Astronomy. Final version available at https://www.nature.com/natastron/