In this work, we present a study of a purely kinetic k-essence model, characterized basically by a parameter α\documentclass[12pt]{minimal}
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\begin{document}$$\alpha $$\end{document} in presence of a bulk dissipative term, whose relationship between viscous pressure Π\documentclass[12pt]{minimal}
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\begin{document}$$\Pi $$\end{document} and energy density ρ\documentclass[12pt]{minimal}
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\begin{document}$$\rho $$\end{document} of the background follows a polytropic type law, Π∝ρλ+1/2\documentclass[12pt]{minimal}
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\begin{document}$$\Pi \propto \rho ^{\lambda +1/2}$$\end{document}, where λ\documentclass[12pt]{minimal}
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\begin{document}$$\lambda $$\end{document}, in principle, is a parameter without restrictions. Analytical solutions for the energy density of the k-essence field are found in two specific cases: λ=1/2\documentclass[12pt]{minimal}
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\begin{document}$$\lambda =1/2$$\end{document} and λ=(1-α)/2α\documentclass[12pt]{minimal}
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\begin{document}$$\lambda =(1-\alpha )/2\alpha $$\end{document}, and then we show that these solutions possess the same functional form as the non-viscous counterpart. Finally, both approaches are contrasted with observational data from type Ia supernova, and the most recent Hubble parameter measurements, and therefore, the best values for the parameters of the theory are found.
