The nature of Przybylski's star: an Ap star model inferred from the light variations and temperature.

New data relevant to the nature of Przybylski's star, RD 101065, are presented. Photographic infrared observations of the hydrogen Paschen lines yield Teff = 7400 + 300 K. Frequency analysis of photometric observations of over 100 cycles of the light variability of RD 101065 indicate a principal period of 12.141 + 0.003 minutes. If this star is on the main sequence, a high pulsational overtone (k 13) may be needed in order to explain the short period. Power spectrum analysis of the light variations indicates that RD 101065 is multiperiodic. It is suggested that an Ap star model can explain all of the known observations of RD 101065. It is argued that previous claims of Fe deficiency are not convincing. Subject headings: stars: abundances - stars: individual - stars: peculiar A - stars: variables