  Debris disks offer valuable insights into the latest stages of circumstellar
disk evolution, and can possibly help us to trace the outcomes of planetary
formation processes. In the age range 10 to 100\,Myr, most of the gas is
expected to have been removed from the system, giant planets (if any) must have
already been formed, and the formation of terrestrial planets may be on-going.
Pluto-sized planetesimals, and their debris released in a collisional cascade,
are under their mutual gravitational influence, which may result into
non-axisymmetric structures in the debris disk. High angular resolution
observations are required to investigate these effects and constrain the
dynamical evolution of debris disks. Furthermore, multi-wavelength observations
can provide information about the dust dynamics by probing different grain
sizes. Here we present new VLT/SPHERE and ALMA observations of the debris disk
around the 40\,Myr-old solar-type star HD\,61005. We resolve the disk at
unprecedented resolution both in the near-infrared (in scattered and polarized
light) and at millimeter wavelengths. Thanks to the new observations, we
propose a solution for both the radial and azimuthal distribution of the dust
grains in the debris disk. We find that the disk has a moderate eccentricity
($e \sim 0.1$) and that the dust density is two times larger at the pericenter
compared to the apocenter. With no giant planets detected in our observations,
we investigate alternative explanations besides planet-disk interactions to
interpret the inferred disk morphology. We postulate that the morphology of the
disk could be the consequence of a massive collision between
$\sim$\,1000\,km-sized bodies at $\sim$\,61\,au. If this interpretation holds,
it would put stringent constraints on the formation of massive planetesimals at
large distances from the star.

Solar and Stellar Astrophysics;Earth and Planetary Astrophysics