Cold gas radial transport in VELA-g3 versus VELA-g6. The top and bottom rows depict the radial mass flux, F_r (in units of ℳ/t_dyn), in VELA-g3 and VELA-g6 disks, respectively, with the left, middle, and right panels, respectively, focusing on streams, non-streams, and all cold gas. The solid lines indicate the medians and the envelopes represent the 16^th − 84^th percentile variations. Rotation-supported disks are identified from all snapshots using the procedure outlined in Section 2.3, and the results from the metallicity- and streamline-based stream selections, as described in Sections 5.2.1 and 5.2.2, are shown in blue and green, respectively. The median cold gas F_r is slightly larger in magnitude in VELA-g6 disks, especially in the outer parts (r > 0.5R_d), likely due to somewhat larger gas fractions in VELA-g6 compared to VELA-g3 (this is because of stronger stellar feedback in VELA-g6, see Fig. A.2). However, F_r is dominated by stream inflows in both VELA-g3 and VELA-g6 disks, especially in the outer parts, irrespective of the strength of stellar feedback or the details of feedback physics.