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Demographic surveys of protoplanetary disks, carried out mainly with ALMA,have provided access to a large range of disk dust masses ($M_{\rm{dust}}$)around stars with different stellar types and in different star-formingregions. These surveys found a power-law relation between $M_{\rm{dust}}$ and$M_{\star}$ that steepens in time, but which is also flatter for transitiondisks (TDs). We performed dust evolution models, which included perturbationsto the gas surface density with different amplitudes to investigate the effectof particle trapping on the $M_{\rm{dust}}-M_{\star}$ relation. Theseperturbations were aimed at mimicking pressure bumps that originated fromplanets. We focused on the effect caused by different stellar and disk massesbased on exoplanet statistics that demonstrate a dependence of planet mass onstellar mass and metallicity. Models of dust evolution can reproduce theobserved $M_{\rm{dust}}-M_{\star}$ relation in different star-forming regionswhen strong pressure bumps are included and when the disk mass scales withstellar mass (case of $M_{\rm{disk}}=0.05\,M_\star$ in our models). This resultarises from dust trapping and dust growth beyond centimeter-sized grains insidepressure bumps. However, the flatter relation of $M_{\rm{dust}}-M_{\star}$ forTDs and disks with substructures cannot be reproduced by the models unless theformation of boulders is inhibited inside pressure bumps. In the context ofpressure bumps originating from planets, our results agree with currentexoplanet statistics on giant planet occurrence increasing with stellar mass,but we cannot draw a conclusion about the type of planets needed in the case oflow-mass stars. This is attributed to the fact that for $M_\star<1\,M_\odot$,the observed $M_{\rm{dust}}$ obtained from models is very low due to theefficient growth of dust particles beyond centimeter-sizes inside pressurebumps.

Hints on the origins of particle traps in protoplanetary disks given by the $M_{\rm{dust}}-M_{\star}$ relation