I have been studying the high resolution line profiles (2400 l/mm grating) from a number of stars and my results are posted here. In this group of projects I am seeking to deduce simple, plausible stellar properties that cause the observed spectral line profiles to be as they are or at least as I measure them.
The reports below represent my current state of understanding (or misunderstanding!) and they may be modified over time, comments would be appreciated (I can be contacted via the RSpec user group).
The studies were conducted using a set of programs I have produced that model a star as a uniformly emitting oblate spheroid with a photosphere that is a single layer in thermal equilibrium.