LIMITS ON MODE-IDENTIFICATIONS IN ROTATING, NON-RADIALLY PULSATING STARS

We present CLEAN time-series analysis of synthetic line profiles obtai ned from a non-radially pulsating stellar model which incorporates eff ects of rotation. Two models (a low-degree l = 2, m = -1; and a high-d egree l = -m - 8) were calculated for a rapidly rotating late 0-type s tar, where the prograde oscillation frequency in the corotating frame of the star is twice that of the stellar rotation frequency. An interp retation of the results based upon the usual slow-rotation assumptions gives a mis-identification of both period and mode of oscillation for the low-degree model, but correctly identifies the NRP characteristic s of the sectorial model. The misidentification of the low-degree mode l has possible implications for previous mode identifications, and we urge caution when analysing the line profile variations of rapidly-rot ating, non-radially pulsating stars.