Screened Scalar Hair and the Weak-Lensing Separation of Black Holes from Neutron Stars in Quadratic $f(R)$ Gravity

RESUMO

Quadratic $f(R)$ gravity carries a massive scalar degree of freedom, the scalaron, whose finite range $\lambda$ screens its influence on the geometry outside a compact object. We show that this screening severs the exterior of a black hole from that of a neutron star of the same mass. The correction to the Schwarzschild metric is Yukawa-suppressed, falling as $e^{-r/\lambda}$ instead of polynomially in the coupling, and is thus invisible to any expansion in powers of that coupling; also, the exterior is intrinsically isotropic, so that inverting the temporal potential alone, as in single-potential solutions, fails to solve ]field equations. Applying the Gauss-Bonnet theorem to this geometry, we find the leading deflection angle to be exactly the general-relativistic $4GM/b$, the scalaron contributions cancelling identically in the combination that bends light. The first correction carries the unfamiliar signature $\lambda^{-1/2}b^{-3/2}e^{-b/\lambda}$, screened beyond the scalaron range and confirmed against direct quadrature to around 20% at $b=4\lambda$, improving to 7% at $b=12\lambda$. What survives is not a difference of degree but of kind. The three ingredients that deliver it, non-analyticity in the coupling, the intrinsically isotropic gauge and the pressure-weighted scalar charge, are here obtained within a single, self-consistent derivation for the first time. A static black hole carries no scalar hair, and lenses precisely as GR requires; a neutron star acquires a scalar charge weighted by the pressure supporting it against collapse, and does not. Weak lensing hence closes as a discriminant of the theory, whilst the horizon, as against a material surface, remains one in principle. The observational advantage lies not in bending angles at large $b$ but in the strong-field imaging of the photon sphere, and in the stellar interior, where the scalar charge is fixed by EoS.