conclusion of this work is given.

Method and data {#Method and data}
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We will simulate the redshift drift data of SKA, and use these mock data to constrain the cosmological models. We will also simulate the redshift drift data of E-ELT, and make comparison and combination with the data of SKA. In order to check how the redshift drift data of SKA will break the parameter degeneracies generated by other cosmological observations, we will also consider the current mainstream observations in this work.

A brief description of the dark energy models
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In this subsection, we will briefly describe the dark energy models employed in the analysis of this work. In a spatially flat universe with a dark energy having an EoS $w(z)$, the form of the Hubble expansion rate is given by the Friedmann equation, $$\begin{aligned}
  E^2(z)&\equiv\frac{H^{2}(z)}{H^{2}_{0}}=\Omega_{\rm m}(1+z)^{3}+\Omega_{\rm r}(1+z)^{4}\\
 & +(1-\Omega_{\rm m}-\Omega_{\rm r})\exp(3 \int^{z}_{0} \frac{{1+w(z')}}{{1+z'}}dz'),
\end{aligned}$$ where $\Omega_{\rm m}$ and $\Omega_{\rm r}$ correspond to the present-day fractional densities of matter and radiation, respectively. Next, we will directly give the expressions of $E(z)$ for the $\Lambda$CDM, $w$CDM, CPL, and HDE models. Note that since we mainly focus on the evolution of the late universe, in the following we shall 