Neutron star models in perturbative f (R) gravity are considered with realistic equations of state. In particular, we consider the FPS and SLy equations of state. The mass-radius relations for f (R) = R+β R(e~(-R/R0) -1) model and for R~2 models with cubic corrections are obtained. In the case of R~2 gravity with cubic corrections, we obtain that at high central densities (ρ > 10ρ_(ns), where ρ_(ns) = 2.7×10~(14) g/cm~3 is the nuclear saturation density), stable star configurations exist. The minimal radius of such stars is close to 9 km with maximal mass ～ 1.9M_⊙ (SLy equation) or to 8.5 km with mass ～ 1.7M_⊙ (FPS equation). This effect can give rise to more compact stars than in GR. If observationally identified, such objects could constitute a formidable signature for modified gravity at astrophysical level.
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机译：扰动F（R）重力中的中子星模型被认为是具有现实状态的现实方程。特别是，我们考虑国家的FPS和狡猾方程。获得F（R）= R +βR（E〜（-R / R0）-1）模型和具有立方校正的R〜2模型的质量半径关系。在具有立方校正的R〜2重力的情况下，我们在高中密度（ρ>10ρ_（ns），其中ρ_（ns）= 2.7×10〜（14）g / cm〜3是核饱和密度），存在稳定的星形配置。最小的这种恒星的半径接近9公里，最大质量〜1.9m_⊙（均匀的方程）或8.5km，质量〜1.7m_ν（FPS方程）。这种效果可以产生比GR更紧凑的恒星。如果观察到鉴定，这些物体可以构成用于在天体物理水平的改性重力的强大签名。
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