  Supermassive stars (SMS) are massive hydrogen objects, slowly radiating their
gravitational binding energy. Such hypothetical primordial objects may have
been the seed of the massive black holes (BHs) observed at the centre of
galaxies. Under the standard picture, these objects can be approximately
described as n=3 polytropes, and they are expected to shine extremely close to
their Eddington luminosity. Once however, one considers the porosity induced by
instabilities near the Eddington limit, which give rise to super-Eddington
states, the standard picture should be modified. We study the structure,
evolution and mass loss of these objects. We find the following. First, the
evolution of SMSs is hastened due to their increased energy release. They
accelerate continuum driven winds. If there is no rotational stabilization,
these winds are insufficient to "evaporate" the objects, such that they can
collapse to form a supermassive BHs, however, they do prevent SMSs from
emitting a copious amount of ionizing radiation. If the SMSs are rotationally
stabilized, the winds "evaporate" the objects until a normal sub-Eddington star
remains, having a mass of a few 100Msun.
