The Multi-periodic Blazhko Modulation of CZ Lacertae

TL;DR

This study provides a detailed analysis of the complex multi-periodic Blazhko modulation in the RRab star CZ Lacertae, revealing two interacting modulation components with changing periods and amplitudes over two seasons.

Contribution

It is the first detailed multi-season study of CZ Lacertae's Blazhko modulation, identifying two distinct modulation periods and their interaction dynamics.

Findings

Two modulation periods (~14.6 d and ~18.6 d) identified.

Modulation frequencies shifted from 5:4 to 4:3 resonance ratio.

Interaction caused beating with a 74-day period.

Abstract

Thorough analysis of the multicolour CCD observations of the RRab-type variable, CZ Lacertae is presented. The observations were carried out in two consecutive observing seasons in 2004 and 2005 within the framework of the Konkoly Blazhko Survey of bright, northern, short-period RRab variables. The O-C variation of CZ Lac indicated that a significant period decrease took place just around the time of the CCD observations. Our data gave a unique opportunity to study the related changes in the pulsation and modulation properties of a Blazhko star in detail. Two different period components ($\approx$14.6 d and $\approx$18.6 d) of the Blazhko modulation were identified. Both modulation components had similar strength. The periods and amplitudes of the modulations changed significantly from the first season to the next, meanwhile, the mean pulsation amplitude slightly decreased. The modulation frequencies were in a 5:4 resonance ratio in the first observing season then the frequencies shifted in opposite directions, and their ratio was close to the 4:3 resonance in the next season. The interaction of the two modulations caused beating with a period of 74~d in the first season, which resembled the 4-yr-long cycle of the $\approx$40-d modulation of RR Lyr. The mean values of the global physical parameters and their changes with Blazhko phase of both modulation components were determined by the Inverse Photometric Method.