Correlation between EUV and activity parameters following the conversion of the value into Ca II H&K chromospheric emission fluxes and following the scaling relations from Linsky et al. (2013, 2014) for F- (red), G- (green), K- (blue), and M-type (magenta) stars. The black line and grey shaded area are the linear fits obtained for F-, G-, and K-type stars (left) and for M-type stars (right) and shown in Fig. 5. The black dots (left) and open blue squares (right) indicate the position of the stars that are both in Linsky et al. (2014) and our sample; the log (EUV∕F_bol) values are from Linsky et al. (2014). For inactive stars, deriving the EUV fluxes from the values by employing the scaling relations from Linsky et al. (2013, 2014) leads to overestimations of about one order of magnitude.