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In this paper, we study a particular type of inflation by using non-localFriedman equations that are somehow derived from the zero levels of stringfield theory and express a tachyonic action. Then, we challenge it by furtherrefining de Sitter (dS) swampland conjecture (FRdSSC) monitoring. Therefore, weinvestigate some quantities, such as potential and Hubble parameters. We alsoconsider slow-roll parameters to examine quantities such as the scalar spectrumindex and the tensor-to-scalar ratio. Using straightforward calculations, weinvestigate this model from the swampland conjecture perspective in terms ofthe cosmological parameters, i.e., ($n_s$), ($r$), and observable data such asPlanck 2018, by constructing some structures such as $(c_1,2-n_s)$ and$(c_1,2-r_s)$. Then, we make a new restriction for this conjecture as$c_12c_22$ and get a limit for this model in the range $c0.0942$. We find thisinflationary model is strongly in tension with the dS swampland conjecture(dSSC), i.e., $c_1=c_2 \neq \mathcal{O}(1)$. So, we shall challenge it with theFRdSSC, which has some free parameters, viz., $a,b>0$, $a+b=1$, and $q>2$. Bysetting these parameters, we examine the compatibility of the mentionedconjecture with this inflationary model. Finally, we infer from this stringfield inflation model that it satisfies the FRdSSC with the constraint of itsfree parameters $a$, $b$, and $q$.

de Sitter Swampland Conjecture in String Field Inflation