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We study the dependence of protoplanetary disk evolution on stellar massusing a large sample of young stellar objects in nearby young star-formingregions. We update the protoplanetary disk fractions presented in our recentwork (paper I of this series) derived for 22 nearby (< 500 pc) associationsbetween 1 and 100 Myr. We use a subsample of 1 428 spectroscopically confirmedmembers to study the impact of stellar mass on protoplanetary disk evolution.We divide this sample into two stellar mass bins (2 M$_{\odot}$ boundary) andtwo age bins (3 Myr boundary), and use infrared excesses over the photosphericemission to classify objects in three groups: protoplanetary disks, evolveddisks, and diskless. The homogeneous analysis and bias corrections allow for astatistically significant inter-comparison of the obtained results. We findrobust statistical evidence of disk evolution dependence with stellar mass. Ourresults, combined with previous studies on disk evolution, confirm thatprotoplanetary disks evolve faster and/or earlier around high-mass (> 2M$_{\odot}$) stars. We also find a roughly constant level of evolved disksthroughout the whole age and stellar mass spectra. We conclude thatprotoplanetary disk evolution depends on stellar mass. Such a dependence couldhave important implications for gas giant planet formation and migration, andcould contribute to explaining the apparent paucity of hot Jupiters aroundhigh-mass stars.

Protoplanetary disk lifetimes vs stellar mass and possible implications for giant planet populations