Abstract
ABSTRACT 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).
Highlights
Protoplanetary discs are the cradle of newborn planets
In Paper I, we presented a series of smoothed particle hydrodynamical (SPH) simulations of a protoplanetary disc disturbed by a single stellar flyby
We assumed the CO is in local thermodynamic equilibrium and a gas temperature equal to the dust temperature computed by MCFOST
Summary
Protoplanetary discs are the cradle of newborn planets. Given typical disc lifetimes – 1 to 10 Myr – planets should form within these systems in less than a few Myr. Numerous radial and azimuthal features such as spirals (Benisty et al 2015, 2017; Perez et al 2016; Huang et al 2018), shadows (Avenhaus et al 2014; Stolker et al 2016; Benisty et al 2018), gaps (ALMA Partnership 2015; Tsukagoshi et al 2016; Andrews et al 2018; Dipierro et al 2018), warps (Casassus et al 2018; Langlois et al 2018; van der Plas et al 2019), horseshoes (van der Marel et al 2013; Boehler et al 2017), and clumps (Dong et al 2018; Gratton et al 2019) have been reported. Such structures are potential signposts of disc–companion interactions (for instance Dong et al 2015; Price et al 2018b; Calcino et al 2019; Poblete, Cuello & Cuadra 2019)
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