Under solar-scaled magnetograms with E_FR ∝ ⟨B★⟩², CME speed and mass rise roughly as v_CME ∝ ⟨B★⟩ and M_CME ∝ ⟨B★⟩^1.5, driven mainly by the upward Lorentz force.
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How Magnetic Field Strength Affects Stellar Coronal Mass Ejection Dynamics
Under solar-scaled magnetograms with E_FR ∝ ⟨B★⟩², CME speed and mass rise roughly as v_CME ∝ ⟨B★⟩ and M_CME ∝ ⟨B★⟩^1.5, driven mainly by the upward Lorentz force.