Debris discs in binaries: morphology and photometric signatures

Context. Since about half of all main-sequence stars reside in multiple star systems, it is important to consider the effect binarity on evolution planetesimal belts these complex systems. Aims. We aim see whether debris evolving between two may be impacted by presence companion and this leaves any detectable signature that could observed with current or future instruments. Methods. a circumprimary parent body (PB) belt placed just inside stability limit we use state-of-the-art DyCoSS code follow coupled dynamical collisional dust produced PB belt. explore several free parameters, such as belt’s mass binary’s ratio well its orbital eccentricity. GraTeR package produce 2D luminosity maps system-integrated spectral energy distributions (SEDs). Results. confirm preliminary result obtained previous studies, which activity, binary perturbations, stellar radiation pressure able place maintain halo small grains dynamically unstable region stars. In addition, identify prominent spatial structures, notably, single spiral arm stretching way from star. also fainter more compact disc around secondary star, non-native feeds off halo. The halo, arm, should resolved images instruments capacities level SPHERE. system whole depleted when compared companion-free case. This depletion an imprint system’s integrated SED, appears colder than for same new finding explain why SED-derived location, r , some unresolved discs-in-binaries places their primary ’forbidden’ stars: indeed, apparent paradox due overestimation using empirical prescriptions are valid case