Alejandro Báez-Rubio, Jesús Martín-Pintado, Clemens Thum, Pere Planesas
Context. The best example of a massive star with an ionized outflow launched from its photoevaporating disk is MWC349A. The large amount of reported radio-continuum and radio-recombination line observations toward this galactic UC-HII region offers a unique possibility to build a model of the ionized envelope of this source. Aims. To understand the physical conditions and kinematics of the ionized region of the circumstellar disk and also of the outflow of MWC349A. Methods. We compared the bulk of radio-continuum maps, radio-recombination line profiles, and the H30alpha centroid map published to date with the predictions of our non-LTE 3D radiative transfer model, MORELI (MOdel for REcombination LInes), which we describe here in detail. Results. Our non-LTE 3D radiative transfer model provides new evidence that the UC-HII region of MWC349A is composed of an ionized circumstellar disk rotating in Keplerian fashion around a star of 38 solar mass, and an ionized outflow expanding with a terminal velocity of 60 km/s and rotating in the same sense as the disk. The model shows that while maser amplification is the dominant process involved for Hn\alpha radio-recombination line (RRL) emission with quantum numbers n<41, stimulated emission is relevant for the emission of RRLs with n>41 up at least the H76alpha line. Conclusions. For the first time, we present a model of MWC349A which satisfactorily explains the vast amount of reported observational data for a very wide range of frequencies and angular resolutions.
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http://arxiv.org/abs/1307.3896
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