In the original version of our article,1 Figs. 8 and 9 contain the following errors:

  • The order of the bottom two legend entries in both Figs. 8 and 9 should be interchanged.

  • The scale on the vertical axis in Fig. 8(a) is incorrect.

  • The velocity profiles in Fig. 9(b) should correspond to a disk diameter downstream rather than a disk radius downstream.

The corrected figures are shown in Figs. 8 and 9, respectively. The caption of Fig. 8 of the original article has been amended to reflect the correct figure reference from Ref. 2. All conclusions in the original article remain unchanged.

FIG. 8.

(a) Pressure p along the r = 0 axis for Re = 130 and three values of Da = 10−9, 2.5 × 10−4, and 10−3, corresponding to regimes I, II, and III, respectively. (b) Axial velocity uz along the r = 0 axis for Re = 130 and Da as in (a). Experimental data in (b) are redrawn from Fig. 7 of Ref. 2.

FIG. 8.

(a) Pressure p along the r = 0 axis for Re = 130 and three values of Da = 10−9, 2.5 × 10−4, and 10−3, corresponding to regimes I, II, and III, respectively. (b) Axial velocity uz along the r = 0 axis for Re = 130 and Da as in (a). Experimental data in (b) are redrawn from Fig. 7 of Ref. 2.

Close modal
FIG. 9.

(a) The streamwise velocity uz profiles across the wake for an axial position z: (a) on the disk’s face and (b) a distance of one disk diameter downstream of the disk’s rear face, for three values of Da = 10−9, 2.5 × 10−4, and 10−3, corresponding to regimes I, II, and III, respectively. The experimental data in (b) are redrawn from Figs. 6(a) and 6(b) of Ref. 2.

FIG. 9.

(a) The streamwise velocity uz profiles across the wake for an axial position z: (a) on the disk’s face and (b) a distance of one disk diameter downstream of the disk’s rear face, for three values of Da = 10−9, 2.5 × 10−4, and 10−3, corresponding to regimes I, II, and III, respectively. The experimental data in (b) are redrawn from Figs. 6(a) and 6(b) of Ref. 2.

Close modal
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Cummins
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I. M.
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The effect of permeability on the flow past permeable disks at low Reynolds numbers
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