¥ There is a
relatively wide variety of line profile morphologies seen in Chandra
and XMM observations of OB stars
¥ By combining
line profile analysis with other diagnostics, it is becoming clear that a
surprising variety of high-energy physical processes are occurring in early-type
stars
¥ Constellation-X:
High(er)-resolution line profile analysis of
short-wavelength lines
Ionization structure of Fe complex
Much better S/N and time coverage (X-ray line
profile variability?)
Vast increases in the number of stars studied (is
there a strong Malmquist bias in the current data?)