2-D Monte Carlo simulations of H I line formation in massive YSO disk winds

Abstract

Massive young stellar objects (YSOs) are powerful infrared H I line emitters. It has been suggested that these lines form in a outflow from a disk surrounding the YSO. Here, new two-dimensional Monte Carlo radiative transfer calculations are described which test this hypothesis. Infrared spectra are synthesised for a YSO disk wind model based on earlier hydrodynamical calculations. The model spectra are in qualitative agreement with the observed spectra from massive YSOs, and therefore provide support for a disk wind explanation for the H I lines. However, there are some significant differences: the models tend to overpredict the Br alpha/Br gamma ratio of equivalent-widths and produce line profiles which are slightly too broad and, in contrast to typical observations, are double-peaked. The interpretation of these differences within the context of the disk wind picture and suggestions for their resolution via modifications to the assumed disk and outflow structure are discussed.

arXiv comment14 pages, 10 figures. Accepted by MNRAS

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