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The lifetime of mm size dust grains, such as chondrules, in the nominal solarnebula model is limited to $\sim 10^{5}$ yr due to an inward drift driven bygas drag. However, isotopic and petrological studies on primitive meteoritesindicate a discrepancy of $\gtrsim 10^{6}$ yr between the formation time ofchondrules and that of chondritic parent bodies. Therefore chondrules shouldsurvive for $\gtrsim 10^{6}$ yr in the solar nebula against the inward driftwithout subsequent growth (i.e., planetesimal formation). Here we investigatethe conditions of the solar nebula that are suitable for the long lifetime ofchondrule-sized dust particles. We take the turbulent strength, the radialpressure gradient force, and the disk metallicity of the solar nebula as freeparameters. For 1 mm-radius-chondrules to survive and keep their size for$\gtrsim 10^{6}$ yr, the suitable condition is a weak turbulence ($\alpha \sim10^{-6}$), a flat radial profile ($\eta \lesssim 10^{-3}$), and a highmetallicity ($Z\sim 0.1$). This condition is qualitatively consistent with thecharacteristics of protoplanetary disks suggested by recent observations. Weeventually propose that planetesimal formation may be induced by the diskevolution, e.g., the inside-out dispersal of the gas component due to the diskwind.

Chondrule survivability in the solar nebula