Blazhko type fundamental-mode RR Lyrae stars in the globular cluster, M3

TL;DR

This study analyzes the properties of Blazhko-type RR Lyrae stars in the globular cluster M3, revealing their modulation characteristics, dependencies on stellar parameters, and temporal nature of the modulation phenomenon.

Contribution

It provides the largest homogeneous dataset of Blazhko stars in a single cluster, detailing their modulation periods, properties, and dependencies on metallicity and stellar parameters.

Findings

Blazhko periods depend on the cluster's metallicity.

Modulation is a temporal property, not permanent in RRab stars.

No modulation detected in the longest-period stars.

Abstract

Blazhko stars from the extended $BVI_{\mathrm C}$ time series of RRab stars in the globular cluster, M3, are analysed. This is the largest sample of Blazhko stars with full details of their Blazhko properties in a homogeneous stellar system. Blazhko periods and light-curve solutions are determined/estimated for 83 fundamental-mode variables. The lack of phase modulation in Oosterhoff-type~II stars and the diminishing relative strength of the modulation in long-period Oosterhoff-type~I stars are the regular tendencies found between the pulsation and modulation properties of Blazko stars. Similarly to previous results, no modulation of the longest-period stars is detected. The onset of the modulation in a previously regular RRab star, and the similar distribution of modulated and non-modulated stars imply that the modulation is a temporal property of RRL stars, which may occur at any time in any RRab star except the coolest ones. Comparing the modulation periods in M3 and in other samples of Blazhko stars, the mean log$(P_{\mathrm {mod}})$ value is found to depend on the metallicity of the system. The separation of the temperature- and radius-change induced variations supports our previous finding that the photometric radius variation does not show any modulation. The pulsation-averaged mean brightness and temperature of Blazhko stars are found to be larger in the large-amplitude phase of the modulation than in the small-amplitude phase. The larger the amplitude of the modulation, the larger changes of the mean parameters are detected.