Mass-gap compact objects (2.5–5 M☉) can be modeled as neutron stars within f(R,T)=R+2λT gravity using the AV18 equation of state with Bowers-Liang anisotropy and strong magnetic fields.
Among these anisotropy pre- scriptions, we select only the Bowers-Liang model [63], as it is one of the most well-known in the literature [89– 91] and references therein
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Structure of Anisotropic Magnetized Neutron Stars in f(R,T) Gravity with Realistic Equation of State
Mass-gap compact objects (2.5–5 M☉) can be modeled as neutron stars within f(R,T)=R+2λT gravity using the AV18 equation of state with Bowers-Liang anisotropy and strong magnetic fields.