  I present the results of radiation-driven mass-loss predictions for hot stars
of all mass. Mass loss is an important aspect for the evolution of massive
stars, the rotational properties of the progenitors of gamma-ray bursts, and is
essential in assessing whether the most massive stars explode as
pair-instability supernovae, or avoid them due to mass loss. As a result, the
rate of mass loss is critical for our understanding of the chemical enrichment
of the Universe. Of particular interest is the question whether luminous blue
variables are the direct progenitors of some supernovae. Although there is a
growing body of evidence to suggest this, it remains as yet unexplained by
state-of-the-art stellar evolution models. Finally, I discuss the relevance of
mass loss for the appearance and rotational properties of hot Horizontal Branch
stars in globular clusters and subdwarf B stars in the field.
