posted on 02.04.2020, 08:51by Nicolas Cuello, Fabien Louvet, Daniel Mentiplay, Christophe Pinte, Daniel J Price, Andrew J Winter, Rebecca Nealon, Francois Menard, Giuseppe Lodato, Giovanni Dipierro, Valentin Christiaens, Matias Montesinos, Jorge Cuadra, Guillaume Laibe, Lucas Cieza, Ruobing Dong, Richard Alexander
Tidal encounters in star clusters perturb discs around young protostars. In Cuello et al., we detailed the dynamical signatures of a stellar flyby in both gas and dust. Flybys produce warped discs, spirals with evolving pitch angles, increasing accretion rates, and disc truncation. Here, we present the corresponding observational signatures of these features in optical/near-infrared scattered light and (sub) millimetre continuum and CO line emission. Using representative prograde and retrograde encounters for direct comparison, we post-process hydrodynamical simulations with radiative transfer methods to generate a catalogue of multiwavelength observations. This provides a reference to identify flybys in recent near-infrared and submillimetre observations (e.g. RW Aur, AS 205, HV Tau and DO Tau, FU Ori, V2775 Ori, and Z CMa).
NC acknowledges financial support provided by FONDECYT grant 3170680. NC and JC acknowledge support from CONICYT project Basal AFB-170002. FL acknowledges the support of the FONDECYT program n° 3170360. This project has received funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No 823823 (DUSTBUSTERS). CP and DJP acknowledge funding from the Australian Research Council via FT170100040, FT130100034, and DP180104235. FMe acknowledges funding from ANR of France under contract number ANR-16-CE31-0013. AJW, RN, GD, and RA acknowledge financial support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 681601). JC and MM acknowledge support from Iniciativa Científica Milenio via the Núcleo Milenio de Formación Planetaria. MM acknowledges financial support from the Chinese Academy of Sciences (CAS) through a CAS-CONICYT Postdoctoral Fellowship administered by the CAS South America Center for Astronomy (CASSACA) in Santiago, Chile. LC acknowledges financial support provided by FONDECYT grant 1171246. The Geryon2 cluster housed at the Centro de Astro-Ingeniería UC was used for the calculations performed in this paper. The BASAL PFB-06 CATA, Anillo ACT-86, FONDEQUIP AIC-57, and QUIMAL 130008 provided funding for several improvements to the Geryon/Geryon2 cluster.
Monthly Notices of the Royal Astronomical Society, Volume 491, Issue 1, January 2020, Pages 504–514, https://doi.org/10.1093/mnras/stz2938