Relation between the bolometric white-light flare energy and the peak GOES-band soft X-ray flux (1–8 Å = 1.55–12.4 keV) for solar and stellar flares. Data for the superflares (E2, E3) from the G-dwarf EK Dra derived in this paper are plotted as red squares. Other data for superflares from G/F-dwarfs (orange circles) are taken from Guarcello et al. (2019). Data for superflares for M/K-dwarfs are taken from Guarcello et al. (2019); Kuznetsov & Kolotkov (2021), and Stelzer et al. (2022). Note that data from Guarcello et al. (2019) have been converted to GOES-band flux and bolometric WLF energy. The solar observational scaling laws from Cliver et al. (2022; dashed line) and Namekata et al. (2017b; solid line), as well as the empirical law from Shibata et al. (2013; dashed–dotted line), are also plotted.