mainly motivated by trying to reproduce pulsar glitches from strange stars. But they did not discuss the formation of such crusts, either. Usov[@usov97] considered a strange star with a crust (or an atmosphere in his term) the mass of which is many orders of magnitude lower than the maximum value \[only $\Delta M\sim (10^{-20}-10^{-19})
M_\odot$\], and studied the X-ray emission properties from such strange stars. He supposed that a strange star is more likely of this type shortly after its birth before the crust mass reaches the maximum. In principle, a pure bare strange star is unlikely to exist in the universe due to various accretion processes. The question is how thick the crust (or atmosphere) could be in reality. In this paper, we will show through some dimensional estimate that newborn strange stars are likely to have much thinner crusts than the maximum values and that they will keep like this through their lifetimes, unless they encounter some special environments that make sufficient accretion possible. The main reasons for such a conclusion are the rapid rotation and the strong mass ejection as discussed below. We note, however, that thick crusts (close to maximum) should be formed in the strange 