¥ 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?)