The chromospheric heating terms cannot be inferred directly from observational datasets. Furthermore, even estimating the thermodynamical state of the plasma usually involves complex NLTE inversion calculations. Therefore, it has been very difficult to quantify in which proportion different heating mechanisms could be operating at different locations of the chromosphere.
One of the most crucial constraints that we can set a any given location are the chromospheric radiative losses, as they represent the energy that (at least) must be replenish in the chromosphere at any given time.
In this talk I will tackle how the spatio-temporal estimates of the radiative losses and other proxies can be used to discriminate what heating mechanisms could potentially be at work from very high spatial-resolution observations of the solar chromosphere.