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To understand in what mass regime star-forming galaxies (SFGs) build upcentral mass concentration most actively, we present a study on theluminosity-weighted stellar age radial gradient ($\nabla_{\rm age}$)distribution of $\sim3600$ low-redshift SFGs using the MaNGA Pipe3D dataavailable in the SDSS DR17. The mean age gradient is negative, with$\nabla_{\rm age}=-0.14$log Gyr/$R_{\rm e}$, consistent with the inside-outdisk formation scenario. Specifically, SFGs with positive $\nabla_{\rm age}$consist of $\sim 28\%$ at log$(M_{*}/M_{\odot})<9.5$, while this fraction risesup to its peak ($\sim 40\%$) near log$(M_{*}/M_{\odot})=10$ and then decreasesto $\sim 15\%$ at log$(M_{*}/M_{\odot})=11$. At fixed $M_{*}$, SFGs withpositive $\nabla_{\rm age}$ typically have more compact sizes and morecentrally concentrated star formation than their counterparts, indicative ofrecent central mass build-up events. These results suggest that the build-up ofcentral stellar mass concentration in local SFGs is mostly active near$M_{*}=10^{10}M_{\odot}$. Our findings provide new insights on the origin ofmorphological differences between low-mass and high-mass SFGs.

Local star-forming galaxies build up central mass concentration most actively near $M_{*}=10^{10}M_{\odot}$