We put together many observational data of SGRs and AXPs and analyze them with the main purpose to remove contradiction between the real age of these objects and their characteristic times of period change. This work indicates that SGRs and AXPs are neutron stars with magnetic fields up to similar to3 x 10(14) G at birth, which is less than the possible value in the existing magnetar model. These neutron stars undergo starquakes and reconnection of magnetic field occurs from time to time. As a result of these processes plasma is ejected from the NS and propeller mechanism starts to work. Due to the propeller effect P increases and tau decreases. Indeed, high P values are observed in SGRs and in half of the AXPs. Then, for a long time NS looses its activity, its P decreases, tau increases and rapid cooling begins. Each NS stage (AXP, SGR, dim) may occur once or several times until the spin period of the neutron star becomes P > 10-12 s. At the transition period to the SCR and AXP stages, the magnetic field component perpendicular to the rotation axis may increase up to 2-3 times. Observational data and mainly the data of AXP1E1048-5937 and DRQNS RX J1308.8+2127 support this idea.