  In connection with a published critique, the author justifies the use of a
motionless homogeneous plane layer of pure hydrogen plasma that is near local
thermodynamic equilibrium (LTE) for analyzing the characteristics of the
radiation from a chromospheric condensation of thickness $\Delta{}z_m=10\text{
km}$ in a gas dynamic model of stellar flares. It is shown that the shock-wave
model of flares proposed by Belova and Bychkov, as opposed to the model of
Kostyuk and Pikelner, has irremovable internal defects owing to exclusion of
the interaction between a thermal wave (temperature jump) and a non-stationary
radiative shock. In particular, this model (a) does not make it possible to
increase the geometric thickness of a chromospheric condensation owing to
divergence of the fronts of the thermal and shock waves during impulsive
heating, (b) cannot provide heating of the chromospheres of red dwarfs over
significant distances, and (c) predicts $\mathrm{H}_\alpha$ line profiles in
conflict with observational data. It is argued that: (a) the shock-wave model
by Belova and Bychkov represents a development of the kinematic model of solar
flares (Nakagawa et al.) and its application to dMe stars, specifically: a
study of the radiative response of the chromosphere of a red dwarf to impulsive
heating in the simplest gas dynamic statement of the problem (a thermal wave is
excluded, a stationary approach is used); (b) in terms of the Kostyuk and
Pikelner model, the regions behind the stationary shock fronts do not
correspond to a chromospheric condensation with time-varying thickness but to
zones in which the plasma relaxes to a state of thermal equilibrium. It is
emphasized that the separation of the Kostyuk and Pikelner model into "thermal"
and "shock-wave" components is fundamentally impossible.
