Three-component magnetic field and solar wind velocity data from the Explorer 33 and 35 spacecraft have been used to study Alfv¿nic fluctuations in the interplanetary medium. We selected 1/2-hour data periods in which the solar wind velocity fluctuations v and the magnetic field fluctuations b were highly correlated, defined by a correlation coefficient ?0.6 for two or more components. Simultaneous observations of these fluctuations by both spacecraft at different locations in interplanetary space enabled us to determine the phase front orientations of these phenomena. We analyzed 56 half-hour data periods and were able to obtain relatively accurate phase information for 33 of them. Using the direction of the phase front relative to the average field as the main criterion for identification, we obtained the following results. (1) The minimum variance method does not give a good estimate of the phase from direction of Alfv¿nic fluctuations. (2) There is a distinct class of Alfv¿nic fluctuations with phase planes nearly parallel of the mean field B0; these could be static structures and/or waves. (3) Most of the fluctuations whose phase planes are not nearly parallel to B0; these could be static structures and/or waves. (3) Most of the fluctuations whose phase planes are not nearly parallel to B0 (i.e., the propagating fluctuations) move neither radially away from the sun nor along B0. (4) The characteristic length of the phase fronts of Alfv¿nic fluctuations is probably significantly larger than 50 RE. (5) Evidence is presented which indicates that tangential discontinuities and possibly other types of static structures are found among Alfv¿nic fluctuations, indicating that Alfv¿nic fluctuations are probably not solely Alfv¿n waves.