Velocity of solar and stellar prominence/filament eruptions (blueshift events) as a function of flare GOES flux (bottom axis) or bolometric WLF energy (top axis). Data for filament/prominence eruptions on the G-dwarf EK Dra are derived from this study and Namekata et al. (2022d). Data for solar filament eruptions are taken from Seki et al. (2021). Data for M-dwarfs, RS CVn, and young stellar objects are taken from Moschou et al. (2019), Inoue et al. (2023), and Maehara et al. (2021). The cyan solid line is a power-law fitting line for all the solar and stellar data. The black dashed line is a line with a power-law index of 1/6, which represents the upper edge of the solar and stellar data (Takahashi et al. 2016).