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We consider the observational signatures of giant impacts between planetaryembryos. While the debris released in the impact remains in a clump for only asingle orbit, there is a much longer lasting asymmetry caused by the fact thatall debris must pass through the collision-point. The resulting asymmetry isstationary, it does not orbit the star. The debris is concentrated in a clumpat the collision-point, with a more diffuse structure on the opposite side. Theasymmetry lasts for typically around 1000 orbital periods of the progenitor,which can be several Myr at distances of ~50 AU. We describe how the appearanceof the asymmetric disc depends on the mass and eccentricity of the progenitor,as well as viewing orientation. The wavelength of observation, which determinesthe grain sizes probed, is also important. Notably, the increased collisionrate of the debris at the collision-point makes this the dominant productionsite for any secondary dust and gas created. For dust small enough to beremoved by radiation pressure, and gas with a short lifetime, this causes theirdistribution to resemble a jet emanating from the (stationary) collision-point.We suggest that the asymmetries seen at large separations in some debris discs,like Beta Pictoris, could be the result of giant impacts. If so this wouldindicate that planetary embryos are present and continuing to grow at severaltens of AU at ages of up to tens of Myr.

Debris from giant impacts between planetary embryos at large orbital radii