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Rapidly decaying slow magnetoacoustic waves are regularly observed in thesolar coronal structures, offering a promising tool for a seismologicaldiagnostics of the coronal plasma, including its thermodynamical properties.The effect of damping of standing slow magnetoacoustic oscillations in thesolar coronal loops is investigated accounting for the field-aligned thermalconductivity and a wave-induced misbalance between radiative cooling and someunspecified heating rates. The non-adiabatic terms were allowed to bearbitrarily large, corresponding to the observed values. The thermalconductivity was taken in its classical form, and a power-law dependence of theheating function on the density and temperature was assumed. The analysis wasconducted in the linear regime and in the infinite magnetic fieldapproximation. The wave dynamics is found to be highly sensitive to thecharacteristic time scales of the thermal misbalance. Depending on certainvalues of the misbalance time scales three regimes of the wave evolution wereidentified, namely the regime of a suppressed damping, enhanced damping wherethe damping rate drops down to the observational values, and acousticover-stability. The specific regime is determined by the dependences of theradiative cooling and heating functions on thermodynamical parameters of theplasma in the vicinity of the perturbed thermal equilibrium. The comparison ofthe observed and theoretically derived decay times and oscillation periodsallows us to constrain the coronal heating function. For typical coronalparameters, the observed properties of standing slow magnetoacousticoscillations could be readily reproduced with a reasonable choice of theheating function.

Damping of slow magnetoacoustic oscillations by the misbalance between heating and cooling processes in the solar corona