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Stellar bow shocks, bow waves, and dust waves all result from the action of astar's wind and radiation pressure on a stream of dusty plasma that flows pastit. The dust in these bows emits prominently at mid-infrared wavelengths in therange 8 to 60 micron. We propose a novel diagnostic method, the tau-etadiagram, for analyzing these bows, which is based on comparing the fractions ofstellar radiative energy and stellar radiative momentum that is trapped by thebow shell. This diagram allows the discrimination of wind-supported bow shocks,radiation-supported bow waves, and dust waves in which grains decouple from thegas. For the wind-supported bow shocks, it allows the stellar wind mass-lossrate to be determined. We critically compare our method with a previous methodthat has been proposed for determining wind mass-loss rates from bow shockobservations. This comparison points to ways in which both methods can beimproved and suggests a downward revision by a factor of two with respect topreviously reported mass-loss rates. From a sample of 23 mid-infraredbow-shaped sources, we identify at least 4 strong candidates forradiation-supported bow waves, which need to be confirmed by more detailedstudies, but no strong candidates for dust waves.

Bow shocks, bow waves, and dust waves. III. Diagnostics