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F.P. Wilkin, S. Lizano (UNAM/CRyA)
The X-wind model for protostellar winds predicts the presence of a wide-angle, low density component in addition to a highly-collimated jet-like core. This wide-angle wind is a key distinction from competing disk wind models, and its presence has yet to be confirmed observationally due to the difficulty of detecting faint emission close-in. Shock interactions between two X-winds in a binary system provide a potential means of distinguishing between competing models of wind launching and collimation. Motivated by the existence of two nearly parallel jets from the binary L1551 IRS 5, we model the collision of two X-winds with parallel symmetry axes. The winds are assumed to be of equal strength, so neglecting orbital motion and considering the poloidal part of the flow, the resulting shocked shell is planar lying between the two stars. Using a thin-shell formalism, we calculate the flow structure within this shocked region.
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Bulletin of the American Astronomical Society, 35#5
© 2003. The American Astronomical Soceity.