Time series analysis of bright TESS RRc stars: Additional modes, phase variations and more

TL;DR

This study analyzes two years of TESS data on 633 RRc stars, revealing prevalent additional non-radial modes, phase variations, and the incidence of the Blazhko effect, advancing understanding of their pulsation behaviors.

Contribution

It identifies new non-radial modes, characterizes phase and amplitude variations, and correlates these phenomena with stellar properties, providing new insights into RRc star pulsations.

Findings

82.8% of stars have additional frequencies beyond the main pulsation

Detected possible $ ext{l}=10$ non-radial modes in some stars

10.4% incidence rate of the Blazhko effect

Abstract

Using two years of data from the TESS space telescope, we have investigated the time series of 633 overtone pulsating field RR Lyrae (RRc) stars. The majority of stars (82.8 per cent) contain additional frequencies beyond the main pulsation. In addition to the frequencies previously explained by the $\ell = 8$ and $\ell = 9$ non-radial modes, we have identified a group of stars where the additional frequencies may belong to the $\ell = 10$ non-radial modes. We found that stars with no additional frequencies are more common among stars with shorter periods, while stars with longer periods almost always show additional frequencies. The incidence rate and this period distribution both agree well with the predictions of recent theoretical models. The amplitude and phase of additional frequencies are varying in time. The frequencies of different non-radial modes appearing in a given star seem to vary on different timescales. We have determined a 10.4 per cent incidence rate for the Blazhko effect. For several stars we have detected continuous annual-scale phase change without significant amplitude variation. This type of variation offers a plausible explanation for the `phase jump' phenomenon reported in many RRc stars. The main pulsation frequency could show quasi-periodic phase and amplitude fluctuations. This fluctuation is clearly related to additional frequencies present in the star: stars with two non-radial modes show the strongest fluctuations, while stars with no such modes show no fluctuations at all. The summation of the phase fluctuation over time may explain the O-C variations that have long been known for many non-Blazhko RRc stars.