This paper investigates the dynamic stability of bumblebee black holes (BHs) under odd parity perturbations. Bumblebee gravity is a theory where a vector field nonminimally couples to the Ricci tensor, and the authors analyze the stability of spherical BH solutions in this framework. They find that bumblebee BHs do not suffer ghost instability, but gradient and tachyonic instabilities can occur when the bumblebee charge exceeds certain values. The existence of these instabilities depends on the nonminimal coupling constant ξ, which must be at least ~4πG for instabilities to occur. The results show that the charge of a bumblebee BH cannot exceed its mass when ξ(ξ - 16πG) > 0, similar to Penrose's cosmic censorship conjecture. The study also compares the constraints from theoretical considerations with recent observations of supermassive BH shadows by the Event Horizon Telescope Collaboration. The authors find that the bumblebee BH stability analysis imposes stronger constraints on the parameter space than the observations. They also analyze the gradient instability of bumblebee BHs using numerical solutions and find that the charge of a bumblebee BH cannot be too large due to the dynamic instabilities. The results are summarized in a table showing the values of |Q|/M and 1 - ξμ_∞² for bumblebee BHs around 0.5κ. The paper concludes that bumblebee BHs cannot carry a vector charge larger than their mass when ξ(ξ - 2κ) > 0.This paper investigates the dynamic stability of bumblebee black holes (BHs) under odd parity perturbations. Bumblebee gravity is a theory where a vector field nonminimally couples to the Ricci tensor, and the authors analyze the stability of spherical BH solutions in this framework. They find that bumblebee BHs do not suffer ghost instability, but gradient and tachyonic instabilities can occur when the bumblebee charge exceeds certain values. The existence of these instabilities depends on the nonminimal coupling constant ξ, which must be at least ~4πG for instabilities to occur. The results show that the charge of a bumblebee BH cannot exceed its mass when ξ(ξ - 16πG) > 0, similar to Penrose's cosmic censorship conjecture. The study also compares the constraints from theoretical considerations with recent observations of supermassive BH shadows by the Event Horizon Telescope Collaboration. The authors find that the bumblebee BH stability analysis imposes stronger constraints on the parameter space than the observations. They also analyze the gradient instability of bumblebee BHs using numerical solutions and find that the charge of a bumblebee BH cannot be too large due to the dynamic instabilities. The results are summarized in a table showing the values of |Q|/M and 1 - ξμ_∞² for bumblebee BHs around 0.5κ. The paper concludes that bumblebee BHs cannot carry a vector charge larger than their mass when ξ(ξ - 2κ) > 0.