  The past decade has witnessed impressive progress in our understanding of the
physical properties of massive stars in the Magellanic Clouds, and how they
compare to their cousins in the Galaxy. I summarise new results in this field,
including evidence for reduced mass-loss rates and faster stellar rotational
velocities in the Clouds, and their present-day compositions. I also discuss
the stellar temperature scale, emphasizing its dependence on metallicity across
the entire upper-part of the Hertzsprung-Russell diagram.
