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outflow. Furthermore the evolutionary path leading to extreme stellar-spin is not well understood. An  important clue lies in the spectral-type distribution of classical Be stars (i.e. the isolated variety) which  is uniform, and those in high mass X-ray binaries (HMXB) which cluster strongly around spectral type  B0 \cite{Negueruela 1998}. \cite{Negueruela1998}.  The presence of the neutron-star companion in HMXB has been shown to affect both the size and density of the disk (e.g. \cite{Zamanov1998}).  Be star disks are very dynamic on timescales of months to years, sometimes exhibiting quasi-periodic