is much larger than the prediction in ZP69. Our solutions exist in such a large mass flux. From their simulation, the mass flux becomes $|j|\sim 0.2\;m_\mathrm{H}\;\mathrm{km\;s^{-1}}(n/0.5\;\mathrm{cm^{-3}})(v/0.4\;\mathrm{km\;s^{-1}})$, where we assume that the accretion velocity to the CNM is comparable to this velocity dispersion. From figure \[fig:sol\_diag\_lowpre\], the corresponding solutions lie in the C-U or C-U-o solutions.

@KI02 have investigated the TI in the shock-compressed region. They found that the velocity dispersion is as large as several km s$^{-1}$. The corresponding mass flux is $|j|\sim 20\;m_\mathrm{H}\;\mathrm{km\;s^{-1}}(n/10\;\mathrm{cm^{-3}})(v/2\;\mathrm{km\;s^{-1}})$ that is larger than the results in @KI06. The pressure of the shock compressed region is larger than $P_\mathrm{max}$, indicting that the two stable phases cannot coexist. In shock compressed regions, the CNM clouds are embedded not by the stable WNM but by the unstable gas that is supplied continuously by shock compression. The C-c solutions in this pressure range $(P>P_\mathrm{max})$ may describe dynamical condensation from the unstable gas to the CNM in shock compression regions.

Curvature Effect
----------------

Our solutions are derived by assuming the plane-parallel geometry. @Netal05 investigated the curvature effect of the transition front by assuming the quasi-steady approximation. They consider the cylindrical and spherical CNM cloud at the centre. In contrast to 