Bumblebee gravity theory has garnered considerable interest in recent years owing to its potential to induce Lorentz symmetry breaking.This paper presents our calculations regarding the interior Tolman-Oppenheimer-Volkoff(TOV)equation of neutron stars under static conditions,using this modified gravity for spherically symmetric ideal fluids.To obtain analytical quantitative results,we applied a simple polytropic model with n=0.Within this model,we analytically derived the mass-radius relationship of neutron stars under the influence of Bumblebee gravity.We found that the Lorentz breaking parameter ℓ can enhance the upper limit of a neutron star's mass.Moreover,we computed the specific relationship between the rotational inertia I and the quadrupole moment Q of neutron stars under the Newtonian limit and the slow-rotation approximation.Our findings indicate that while the Lorentz breaking parameter ℓ does not change the square proportionality relationship of the dimensionless(I)and(Q),it does indeed modify their proportionality coefficient.Our analytical results provide potential theoretical support for testing the breaking of Lorentz symmetry.
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