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Paper: The Photoionized Disk Wind in MWC 349AOrigin of the photo-ionized wind in MWC349A
Volume: 508, The B[e] Phenomenom: Forty Years of Studies
Page: 279
Authors: Báez-Rubio, A.; Martín-Pintado, J.
Abstract: Establishing how dense photo-ionized winds around stars are formed is key to understanding which physical mechanisms have an important role in the evolution of their circumstellar disks. In the case of the massive star MWC 349A, the extensive research carried out since the discovery of its hydrogen recombination lines has lead to a profound knowledge of the characteristics of the system formed by its ionized wind and disk. We present a summary of the current knowledge of their kinematics, which suggests that its dense wind is formed by photoevaporation of the circumstellar disk at a distance of ∼ 24 AU from the central star. We briefly discuss the reasons why disk-wind models are favored because of the radius where its launching occurs. Finally, we compare our results with the recent discovery of maser recombination lines toward another B[e] star, MWC 922, by Sanchez Contreras et al. (in prep.). This finding opens new prospects for studying the origin of winds around stars showing the B[e] phenomenon.
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