The large-scale properties of 19 flare-associated solar wind disturbances observed by Vela 3 and Vela 4 satellites between August 1965 and June 1967 have been examined. It is generally found that the solar wind flow speed rises above the value measured immediately after the shock at the leading edge of such disturbances and remains elevated for at least 1 day. The mass and energy fluxes may either rise or fall after the discontinuous change at the shock. Integration of the excess of these fluxes above the preshock or ambient level gives the total mass and energy in the interplanetary disturbance. The average mass is found to be 3×1016 g; the average energy (at 1 AU) is 5×1031 ergs. Both the mass and energy are smaller for disturbances in which the energy flux falls after the shock than for disturbances in which it rises. Both quantities are larger for disturbances observed in early 1967 than for those observed in late 1965, thus suggesting that the mass and energy deposited in the solar wind by individual flares increased with the rise in solar activity during the period under discussion. The energy released by the flare (obtained by correcting for the solar gravitational potential at 1 solar radius) is found to be proportional to the mass released, despite variation of more than an order of magnitude in both quantities.