Scalar and vector velocity differences between helium and hydrogen ions in the solar wind measured with the Los Alamos plasma analyzers on Imp 6 and 7 are presented and interpreted. From the bulk speeds and azimuthal components of flow direction for both types of ions the ecliptic projection of the helium to hydrogen velocity difference vector vop is determined. Short-term and long-term average properties of this vector, at time contrasted with the more usually reported bulk speed difference vo-vp, are principal subjects of this paper. The vector is usually found aligned with the proton heat flux vector Qp and therefore is directed predominantly outward from the sun. Sometimes preceding high-speed streams and during fluctuations the vector is directed back toward the sun; i.e., vp>vo. There is a statistical correlation between the magnetude of vop and the wind speed: empirically, ‖vop?0.08vp-23 for vp?420 km s-1. During high-speed streams, ‖v&agr;p‖ is often 25 or 30 km s-1 and on rare occasions as large as 80 km s-1, while at lower wind sppeds it is <10 km s-1. In high-speed streams or in other magnetically disturbed regions the vector difference magnitude often remains nearly constant, while the bulk speed difference undergoes large changes as the difference vector rotates in alignment with B. The underlying physical causes of the He and H speed differences remain undetermined.