  The turbulent environment from which stars form may lead to misalignment
between the stellar spin and the remnant protoplanetary disk. By using
hydrodynamic and magnetohydrodynamic simulations, we demonstrate that a wide
range of stellar obliquities may be produced as a by-product of forming a star
within a turbulent environment. We present a simple semi-analytic model that
reveals this connection between the turbulent motions and the orientation of a
star and its disk. Our results are consistent with the observed obliquity
distribution of hot Jupiters. Migration of misaligned hot Jupiters may,
therefore, be due to tidal dissipation in the disk, rather than tidal
dissipation of the star-planet interaction.
