Non-radial pulsation in first overtone Cepheids of the Small Magellanic Cloud

TL;DR

This study analyzes photometric data of 138 first overtone Cepheids in the Small Magellanic Cloud, revealing non-radial pulsations with complex frequency patterns and subharmonic power excess, suggesting a common pulsation mechanism with RR Lyrae stars.

Contribution

It provides the first detailed analysis of non-radial pulsations in SMC Cepheids, supporting the excitation of high-degree non-radial modes as the underlying cause.

Findings

Detection of additional variability with period ratios 0.60-0.65.

Observation of power excess at half the frequency in 35% of stars.

Variation of pulsation amplitude and phase over time.

Abstract

We analyse photometry for 138 first overtone Cepheids from the Small Magellanic Cloud, in which Optical Gravitational Lensing Experiment (OGLE) team discovered additional variability with period shorter than first overtone period, and period ratios in the (0.60, 0.65) range. In the Petersen diagram these stars form three well separated sequences. The additional variability cannot correspond to other radial mode. This form of pulsation is still puzzling. We find that amplitude of the additional variability is small, typically 2-4 per cent of the first overtone amplitude, which corresponds to 2-5 mmag. In some stars we find simultaneously two close periodicities corresponding to two sequences in the Petersen diagram. The most important finding is the detection of power excess at half the frequency of the additional variability (at subharmonic) in 35 per cent of the analysed stars. Interestingly, power excess at subharmonic frequency is detected mostly for stars of the middle sequence in the Petersen diagram (74 per cent), incidence rate is much lower for stars of the top sequence (31 per cent), and phenomenon is not detected for stars of the bottom sequence. The amplitude and/or phase of the additional periodicities strongly vary in time. Similar form of pulsation is observed in first overtone RR Lyrae stars. Our results indicate that the nature and cause of this form of pulsation is the same in the two groups of classical pulsators; consequently, a common model explaining this form of pulsation should be searched for. Our results favour the theory of the excitation of non-radial modes of angular degrees 7, 8 and 9, proposed recently by Dziembowski.