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Understanding how young stars gain their masses through disk-to-staraccretion is of paramount importance in astrophysics. It affects our knowledgeabout the early stellar evolution, the disk lifetime and dissipation processes,the way the planets form on the smallest scales, or the connection tomacroscopic parameters characterizing star-forming regions on the largest ones,among others. In turn, mass accretion rate estimates depend on the accretionparadigm assumed. For low-mass T Tauri stars with strong magnetic fields thereis consensus that magnetospheric accretion (MA) is the driving mechanism, butthe transfer of mass in massive young stellar objects with weak or negligiblemagnetic fields probably occurs directly from the disk to the star through ahot boundary layer (BL). The intermediate-mass Herbig Ae/Be (HAeBe) starsbridge the gap between both previous regimes and are still optically visibleduring the pre-main sequence phase, thus constituting a unique opportunity totest a possible change of accretion mode from MA to BL. This review deals withour estimates of accretion rates in HAeBes, critically discussing the differentaccretion paradigms. It shows that although mounting evidence supports that MAmay extend to late-type HAes but not to early-type HBes, there is not yet aconsensus on the validity of this scenario versus the BL one. Based on MA andBL shock modeling, it is argued that the ultraviolet regime could significantlycontribute in the future to discriminating between these competing accretionscenarios.

On the Mass Accretion Rates of Herbig Ae/Be Stars. Magnetospheric Accretion or Boundary Layer?