  Magnetohydrodynamic turbulence is a ubiquitous phenomenon in solar physics,
plasma physics and astrophysics and governs many properties of the flows of
well-conductive fluids. Recently, conflicting spectral slopes for the inertial
range of MHD turbulence has been reported by different groups. Varying spectral
shapes from earlier simulations hinted at a wider spectral locality of MHD,
which necessitated higher resolution simulations and careful and rigorous
numerical analysis. In this Letter we present two groups of simulations with
resolution up to 4096^3 that are numerically well-resolved and has been
analyzed with exact and well-tested method of scaling study. Our results from
both simulation groups indicate that the power spectral slope for all
energy-related quantities, such as total energy and residual energy are around
-1.7, close to Kolmogorov's -5/3. This suggests that residual energy is the
constant fraction, 0.15+-0.03 of the total energy and that in asymptotic regime
magnetic and kinetic spectra have the same scaling. The -1.5 slope for energy
and -2 slope for residual energy suggested by other groups seems to be
completely inconsistent with numerics.
