  To simulate the energy balance of coronal plasmas on macroscopic scales, we
often require the specification of the coronal heating mechanism in some
functional form. To go beyond empirical formulations and to build a more
physically motivated heating function, we investigate the
wave-turbulence-driven (WTD) phenomenology for the heating of closed coronal
loops. Our implementation is designed to capture the large-scale propagation,
reflection, and dissipation of wave turbulence along a loop. The parameter
space of this model is explored by solving the coupled WTD and hydrodynamic
evolution in 1D for an idealized loop. The relevance to a range of solar
conditions is also established by computing solutions for over one hundred
loops extracted from a realistic 3D coronal field. Due to the implicit
dependence of the WTD heating model on loop geometry and plasma properties
along the loop and at the footpoints, we find that this model can significantly
reduce the number of free parameters when compared to traditional empirical
heating models, and still robustly describe a broad range of quiet-sun and
active region conditions. The importance of the self-reflection term in
producing relatively short heating scale heights and thermal nonequilibrium
cycles is also discussed.
