Abstract: When the velocity of the solar wind is accelerated to Alfven speed u_A, Landau damping of original kinetic Alfven waves subspends and the kinetic Alfven wave is excited second time. The velocity of propagation of newly excited Alfven waves with the wind is U+u_A,the velocity of propagation against the wind is U-_A, the former suffers Landau damping and the latter gives Z⁺ mode and has no damping. The interplanetary Alfvenic turbulence is divided into three regions: dissipative region of turbulence(R<0.2AU), re-exciting region (0.2AU0.4AU), and an explanation of the turbulence spectrum features in different region is given. Based on the re-exciting and damping of the kinetic Alfven wave, the fact of higher temperature of proton in high speed stream of the solar wind is explained in this paper.