  We consider two non-canonical scalar fields (tachyon and DBI) with E-model
type of the potential. We study cosmological inflation in these models to find
possible $\alpha$-attractors. We show that similar to the canonical scalar
field case, in both tachyon and DBI models there is a value of the scalar
spectral index in small $\alpha$ limit which is just a function of the e-folds
number. However, the value of $n_{s}$ in DBI model is somewhat different from
the other ones. We also compare the results with Planck2015 TT, TE, EE+lowP
data. The reheating phase after inflation is studied in these models which
gives some more constraints on the model's parameters.
