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This work aims to derive accretion rates for a sample of 38 HAeBe stars. Weapply magnetospheric accretion (MA) shock modelling to reproduce the observedBalmer excesses. We look for possible correlations with the strength of theHalpha, [OI]6300, and Brgamma emission lines.  The median mass accretion rate is 2 x 10^-7 Msun yr^-1 in our sample. Themodel fails to reproduce the large Balmer excesses shown by the four hotteststars (T* > 12000 K). We derive Macc propto M*^5 and Lacc propto L*^1.2 for oursample, with scatter. Empirical calibrations relating the accretion and theHalpha, [OI]6300, and Brgamma luminosities are provided. The slopes in ourexpressions are slightly shallower than those for lower mass stars, but thedifference is within the uncertainties, except for the [OI]6300 line. TheHalpha 10% width is uncorrelated with Macc, unlike for the lower mass regime.The mean Halpha width shows higher values as the projected rotationalvelocities of HAe stars increase, which agrees with MA. The accretion ratevariations in the sample are typically lower than 0.5 dex on timescales of daysto months, Our data suggest that the changes in the Balmer excess areuncorrelated to the simultaneous changes of the line luminosities.  The Balmer excesses and Halpha line widths of HAe stars can be interpretedwithin the context of MA, which is not the case for several HBes. The steeptrend relating Macc and M* can be explained from the mass-age distributioncharacterizing HAeBe stars. The line luminosities used for low-mass objects arealso valid to estimate typical accretion rates for the intermediate-mass regimeunder similar empirical expressions. However, we suggest that several of thesecalibrations are driven by the stellar luminosity.

Accretion rates and accretion tracers of Herbig Ae/Be stars