Mass accretion rates measured from the Hα (left top panel), Hβ (right top panel), He i λ5876 Å (left bottom panel), and He i λ6678 Å (right bottom panel) lines versus mass. Vertical bars connect the minimum and maximum values of Ṁ_acc obtained per each star at different epochs. Stars are divided into high Hα emitters (EW_Hα > 10 Å; grey bars) and low Hα emitters (EW_Hα < 10 Å; orange bars), i.e., stars where the line emission cannot be unambiguously attributed to accretion activity, as it is most likely caused by chromospheric activity. The dashed line shows the relation obtained by Herczeg & Hillenbrand (2008) for Taurus members. The highest Ṁ_acc values in the first and fourth panels refer to the early-type star DK Cha. The lower number of points in the Hβ and He i plots is due to two reasons: absence of the line in the given star or line out of the wavelength range (see Table 5).