Lh. Auer et G. Koenigsberger, LINE-PROFILE VARIATIONS FROM ATMOSPHERIC ECLIPSES - CONSTRAINTS ON THE WIND STRUCTURE IN WOLF-RAYET STARS, The Astrophysical journal, 436(2), 1994, pp. 859-870
Binary systems in which one of the components has a stellar wind may p
resent a phenomenon known as ''wind'' or ''atmospheric eclipse,'' in w
hich that wind occults the luminous disk of the companion. The enhance
d absorption profile, relative to the spectrum at uneclipsed orbital p
hases, can be modeled to yield constraints on the spatial structure of
the eclipsing wind. A new, very efficient approach to the radiative t
ransfer problem, which makes no requirements with respect to monotonic
ity of the velocity gradient or the size of that gradient, is presente
d. The technique recovers both the comoving frame calculation and the
Sobolev approximation in the appropriate limits. Sample computer simul
ations of the line profile variations induced by wind eclipses are pre
sented. It is shown that the location of the wind absorption features
in frequency is a diagnostic tool for identifying the size of the wind
acceleration region. Comparison of the model profile variations with
the observed variations in the W-R+6 binary system V444 Cyg illustrate
how the method can be used to derive information on the structure of
the wind of the W-R star and constrain the size of the W-R core radius
.