Mass M_CME (a) and kinetic energy E_k (b) plotted as functions of flaring bolometric energy (bottom horizontal axis) and X-ray energy emitted in the GOES band (top axis) for solar and stellar filament and prominence eruptions and CMEs. The solar CME data (filled sky-blue circles) are derived from Yashiro & Gopalswamy (2009). The solar prominence and filament eruptions and surges (green plus signs) are from Namekata et al. (2024), originally taken from Namekata et al. (2021) and Kotani et al. (2023). The dashed and dotted lines are trend fits for the solar CMEs expressed as $M_{\mathrm{CME}}\propto E_{\mathrm{X}}^{0.59}$ and E_k ∝ E^1.05 (Drake et al. 2013) and $M_{\mathrm{CME}}\propto E_{\mathrm{X}}^{0.7}$ (Aarnio et al. 2012). (c) Comparison between the velocity and length scales of the filament eruptions on the Sun and UX Ari. The solid black line indicates a threshold (see Seki et al. 2021).