  Disks are a natural outcome of the star formation process in which they play
a crucial role. Luminous, massive stars of spectral type earlier than B4 are
likely to be those that benefit most from the existence of accretion disks,
which may significantly reduce the effect of radiation pressure on the
accreting material. The scope of the present contribution is to review the
current knowledge about disks in young high-mass (proto)stars and discuss their
implications. The issues of disk stability and lifetime are also discussed. We
conclude that for protostars of less than ~20 solar masses, disks with mass
comparable to that of the central star are common. Above this limit the
situation is unclear and there are no good examples of proto O4-O8 stars
surrounded by accretion disks: in these objects only huge, massive, toroidal,
non-equilibrium rotating structures are seen. It is clear on the other hand
that the observed disks in stars of 10-20 solar masses are likely to be
unstable and with short lifetimes.
