initial values of the energy dissipation and the baryon diffusion currents are set to zero to allow comparison of the effects of those processes coming from hydrodynamic evolution.

The kinetic freeze-out is estimated using the Cooper-Frye formula [@Cooper:1974mv] with off-equilibrium corrections to the phase-space distribution functions [@Teaney:2003kp; @Monnai:2009ad]. It reads $$\begin{aligned}
E_i\frac{dN^i}{d^3p} = \frac{g_i}{(2\pi)^3} \int_\Sigma p_i^\mu d\sigma_\mu (f^0_i + \delta f_i), \label{eq:CF}\end{aligned}$$ where $g_i$ is the degeneracy, $\Sigma$ is the freeze-out hypersurface, and $d\sigma_\mu$ is the freeze-out hypersurface element. $f_i^0$ is the equilibrium (Bose-Einstein or Fermi-Dirac) phase-space distribution function for the $i$-th particle species and $\delta f_i$ is the off-equilibrium distortion of the distribution function. The expression of $\delta f$ in the Landau and the Eckart frames are shown in Appendix \[sec:B\]. The hypersurface is determined with the freeze-out energy density $e_\mathrm{f} = 0.4$ GeV/fm$^3$.

Space-time evolution {#sec4B}
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![The space-time rapidity dependences of (a) the entropy density and (b) the net baryon density at the initial time (thin solid line) and those after ideal (thick solid line), baryon diffusive (dashed line), and energy dissipative (dotted line) hydrodynamic evolutions at $\tau = 20$ fm/$c$.[]{data-label="fig:1"}](entropy.pdf "fig:"){width="3.3in"} ![The space-time rapidity dependences of (a) the entropy density and (b) the net baryon density 