Anisotropic stellar solutions in torsion-trace gravity under Karmarkar condition

In this paper, we formulate exact anisotropic interior solutions of the Einstein field equations preserving spherically symmetric geometry in the context of [Formula: see text] gravity. To make the system close, we consider a linear function in torsion scalar [Formula: see text] and trace of energy–momentum tensor [Formula: see text], and employ the well-known Karmarkar condition with metric potential of the form [Formula: see text]. We consider standard data of some well-known compact star models (Vela X-1, PSR J1614-2230, Cen X-3 and EXO 1785-248) to estimate the unknown model parameters. We perform physical analysis of the developed model in detail, which includes density profile, pressure profile, anisotropy factor, mass function, gravitational/surface redshift, compactness factor, energy bounds, stability criteria, and the equilibrium condition. The analysis leads us to conclude that solutions are well-behaved and physically viable.

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