Abstract
The variety of the observed Ha line profiles in the spectra of Herbig Ae/Be (HAEBE) stars firstly described by Finkenzeller & Mundt (1984) demanded, as believed, the same or almost the same variety of kinematical models for their interpretation (Catala 1994). Traditionally, the outflow of matter is considered as the main physical process in HAEBE stars and the star AB Aur which exhibits strong P Cygni profiles in many emission lines is frequently considered as the prototype of HAEBE stars.
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