Rindler firewall can be generated by a uniformly accelerated mirror and we conjecture that a black hole firewall could be squeezed. We conclude in Sec. \[conclusion\]. In this paper, we take the unit $\hbar = c =1$.

Rindler modes and Unruh modes {#RindlerUnruh}
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In this section we describe the relations between Rindler modes and Unruh modes, which act as the foundation of our quantum circuit model. We begin with a brief review of the three ways of quantizing a massless scalar field $\hat{\Phi}$ in $(1+1)$-dimensional Minkowski spacetime (for comprehensive reviews, see [@Takagi86; @Crispino08]).

A massless scalar field $\hat{\Phi}$ satisfies the Klein-Gordon equation $\Box \hat{\Phi} = 0$, where the d’ Alembertian $\Box \equiv  (\sqrt{-g})^{-1} \partial_{\mu} [\sqrt{-g}g^{\mu\nu} \partial_{\nu}]$ and $g_{\mu\nu}$ is the metric of the spacetime [@Birrell82]. In the inertial frame, Minkowski coordinates $(t, x)$ are used and the metric $g_{\mu\nu} = \eta_{\mu\nu} = \text{diag}\{-1, +1\}$. The scalar field $\hat{\Phi}$ can be quantized in the standard way, $$\label{MinkowskiMode}
\hat{\Phi} = \int d k \big(\hat{a}_{1k} u_{1k}  + \hat{a}_{2k} u_{2k} +  \text{h.c.}  \big),$$ where h.c. represents Hermitian conjugate, $u_{1k}~(u_{2k})$ are single-frequency left-moving (right-moving) mode functions $$u_{1k}(V) = (4 \pi k)^{-1/2} e^{-i k V}, \,\,\,\,\,\, u_{2k}(U) =(4 \pi k)^{-1/2} e^{-i k U},$$ with $V 