“…The period of 26.7 d can then be interpreted as period of relative rotation of sunspots at mean latitude of their appearance j ¼ 15 with T 1 ¼ 25:28 d, combined with the rotation of the Sun at the base of convection zone, with T ¼ 1:3 yr at the same latitudes (Howe et al, 2000). Taking T 2 ¼ 1:3 yr ¼ 474:81 d and 1=T 12 ¼ 1=T 1 AE 1=T 2 , where alternative signs apply because rotation at T ¼ 1:3 yr occurs in opposite phase below and above the base of the convection zone (Howe et al, 2000), we obtain T 12 ¼ 26:7 or 24.0 d. We have previously found evidence that the 24 d period exists in IMF data measured in the solar wind near the Mars on board Phobos-2 (Kuznetsova et al, 1995;Tsirulnik et al, 1997a).…”