High-speed streams in the solar wind are located with respect to interplanetary magnetic sectors, and their location in the sector is analyzed. The relation to the sector taken as a whole is clearer than the relation to sector boundaries. The streams occur preferentially near the center of the sector. Although high-speed streams, as do sector boundaries, show a clear pattern of recurrence with solar rotation and although they are about equally frequent in the period studied (1965--1971), there is no one-to-one relation between them; sectors with no stream or with more than one stream are common. Longer sectors contain more streams, showing that streams occur at a certain rate per unit time rather than at a constant number per sector.