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State-of-the-art MHD calculations reveal acceptable agreement withobservational data for the height profile of the temperature $T(h)$ in thetransition region of solar corona. Simultaneously, the velocity of the solarwind $U(h)$ has also been calculated. The developed method gives thepossibility at given frequency dependent spectral density of Alfv\'en waves(AW) coming from chromosphere $\mathcal{W}(\omega)$ to calculate both heightprofiles $T(h)$ and $U(h)$. In agreement with the concepts of the self-inducedopacity of plasma with respect of AW, the narrow width $\lambda$ of thetransition region is determined by the fast temperature increase of theviscosity $\eta(T,B)$. After more than 70 years of development of Solarphysics, the Alfv\'en hypothesis of heating of the solar corona by AW hasremained without alternatives; none of other mechanisms can explain $ab$$initio$ the value of $\lambda$. The performed MHD analysis explains the heightdependence of the non-thermal broadening of the chromospheric spectral linesand predicts angular dependence of this broadening with respect of position insolar disc. One can expect significant impact of MHD analysis in theinterpretation of the long expected data from Parker Solar Probe.

The Theory of Heating of the Solar Corona and Launching of the Solar Wind by Alfv\'en Waves