  We investigate the possibility of erosion of planetesimals in a
protoplanetary disk. We use theory and direct numerical simulations (Lattice
Boltzmann Method) to calculate the erosion of large -- much larger than the
mean-free-path of gas molecules -- bodies of different shapes in flows. We find
that erosion follows a universal power-law in time, at intermediate times,
independent of the Reynolds number of the flow and the initial shape of the
body. Consequently, we estimate that planetesimals in eccentric orbits, of even
very small eccentricity, rapidly (in about hundred years) erodes away if the
semi-major axis of their orbit lies in the inner disk -- less than about $10$
au. Even planetesimals in circular orbits erode away in approximately ten
thousand years if the semi-major axis of their orbits are $\lessapprox 0.6$au.
