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[105.11] Monte-Carlo Models of Accretion Disks around Young Stars in the Orion Nebula

T. Le Blanc (Fisk Univ.), K.G. Stassun (Vanderbilt Univ.), E.L.N. Jensen (Swarthmore College)

Current theory suggests that the accretion disks around classical T-Tauri stars regulate the spins of these stars, by way of the magnetic field lines. These field lines extend from the star into the accretion disk, and in effect "locking" the angular velocity of the star to that of the material at the inner edge of the disk (the truncation radius). This disk shows up as an IR excess in the spectral energy distribution (SED) emitted by the star. The truncation radius of the disk can be determined from the observed SED. According to theory, this truncation radius can be a key parameter in the regulation of the angular momentum evolution of the star.

We are currently using a Monte-Carlo code to model the SEDs of some 600 young stars in the Orion Nebula. By comparing these models to upcoming observations of these young stars, we will test whether the truncation radii of the stars are consistent with that predicted by theory.

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Bulletin of the American Astronomical Society, 36 5
© 2004. The American Astronomical Society.