[en] During large flares, the Sun ejects magnetic bubbles which are then convected by the solar wind into the interstellar medium. The bubbles partake of the spherical expansion of the solar wind and grow to spatial scales comparable to the gyroradii of 10²--10³ GeV cosmic rays. Assuming that most stars leave behind a wake of magnetic bubbles in the interstellar medium, and that the rate of bubble production is comparable to the solar rate, 10²--10³ GeV and possibly higher energy cosmic rays will be well scattered and have mean free paths consistent with the compound diffusion theory. Particular choices for the scale length spectrum of bubbles yield mean free paths which depend only weakly on cosmic-ray energy