Abstract
We examine the dynamics of warm inflation in the context of modified teleparallel gravity, \(\mathtt f(T,\mathcal T)\) , focusing on the strong dissipative regime ( \(r>1\) ). Two representative inflationary potentials chaotic \((V(\vartheta)\propto\vartheta^n)\) and natural \((V(\vartheta)=\Lambda^4[1+\cos(\vartheta/f)])\) are analyzed considering both constant and field-dependent dissipation coefficients. For the chaotic potential with constant dissipation, the scalar spectral index \(n_{\mathrm s}\) remains nearly insensitive to the model exponent \(n\) , while the tensor-to-scalar ratio \(R\) shows a clear dependence. For typical choices, \(n_{\mathrm s}\simeq 0.965-0.970\) and \(R\lesssim 0.07\) , consistent with Planck \(2018+\mathrm{BK}18\) bounds at \(95\%\) C.L. With a variable dissipation coefficient, only one specific chaotic scenario satisfies observational limits, with the energy scale adapting to model parameters. For the natural potential, \(\mathtt f(T,\mathcal T)\) corrections play a key role, adjusting both \(n_{\mathrm s}\) and \(R\) to fall within the Planck \({2018+\mathrm{BK}18}\) allowed ranges while permitting the symmetry-breaking scale \(f\) to remain sub-Planckian. These results contrast with cold inflation models, where similar \(\mathtt f(\mathcal R,T)\) corrections fail to render the potentials compatible with observations. Our study suggests that exploring alternative \(f(T,\mathcal T)\) forms and revisiting previously excluded potentials could further illuminate the viability of warm inflation scenarios.
