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Supersonic turbulence in the interstellar medium (ISM) is believed to decayrapidly within a flow crossing time irrespective of the degree ofmagnetization. However, this general consensus of decaying magnetohydrodynamic(MHD) turbulence relies on local isothermal simulations, which are unable totake into account the roles of global structures of magnetic fields and theISM. Utilizing three-dimensional MHD simulations including interstellar coolingand heating, we investigate decaying MHD turbulence within cold neutral mediumsheets embedded in warm neutral medium. Early evolution of turbulent kineticenergy is consistent with previous results for decaying compressible MHDturbulence characterized by rapid energy decay with a power-law form of$E\propto t^{-1}$ and by short decay time compared to a flow crossing time. Ifinitial magnetic fields are strong and perpendicular to the sheet, however,long-term evolution of the kinetic energy shows that a significant amount ofturbulent energy ($\sim 0.2E_0$) still remains even after ten flow crossingtimes for models with periodic boundary conditions. The decay rate is alsogreatly reduced as the field strength increases for such initial and boundaryconditions, but not if the boundary conditions are that for a completelyisolated sheet. We analyze velocity power spectra of the remaining turbulenceto show that in-plane, incompressible motions parallel to the sheet dominate atlater times.

Long-Term Evolution of Decaying MHD Turbulence in the Multiphase ISM