Dependence of clump migration on ω in disks with M_MCC = 1 M_⊙ and T_MCC = 15 K. Using different line styles, we differentiate different ω values. Each pair of the lines with the same style represents the time evolution of the radial positions of the clumps forming at the inner and the outer boundary of the fragmentation region at t = 3.5 × 10⁵ yr (time when the collapse of the parent cloud core ends) in a protoplanetary disk with a specific ω. The pairs of the dotted, short-dotted, solid, short-dashed, and dashed lines represent the evolution of the radial positions of clumps forming in disks with ω = 1.5 × 10⁻¹⁴ s⁻¹, 2.0 × 10⁻¹⁴ s⁻¹ 2.8 × 10⁻¹⁴ s⁻¹ 5.0 × 10⁻¹⁴ s⁻¹ and 8.0 × 10⁻¹⁴ s⁻¹ respectively. The other information is the same as Fig. 1.