Multi-site, multi-year monitoring of the oscillating Algol-type eclipsing binary CT Her

TL;DR

This study presents multi-year, multi-site photometric observations of the eclipsing binary CT Her, revealing complex pulsation frequencies and amplitude variability, and discusses implications for binary and pulsation evolution.

Contribution

It provides detailed pulsation analysis of CT Her, identifying multiple frequencies and amplitude changes, and combines photometry with radial velocity data for comprehensive system modeling.

Findings

Detected up to eight significant pulsation frequencies.

Confirmed rapid pulsations with a main period of 27.2 minutes.

Observed amplitude variability over 1-2 years.

Abstract

We present the results of a multi-site photometric campaign carried out in 2004-2008 for the Algol-type eclipsing binary system CT Her, the primary component of which shows Delta Scuti-type oscillations. Our data consist of differential light curves collected in the filters B and V which have been analysed using the method of Wilson-Devinney (PHOEBE). After identification of an adequate binary model and removal of the best-matching light curve solution, we performed a Fourier analysis of the residual B and V light curves to investigate the pulsational behaviour. We confirm the presence of rapid pulsations with a main period of 27.2 min. Up to eight significant frequencies with semi-amplitudes in the range 3 to 1 mmag were detected, all of which surprisingly lie in the frequency range 43.5-53.5 c\d. This result is independent from the choice of the primary's effective temperature (8200 or 8700 K) since the light curve models for the binary are very similar in both cases. This is yet another case of a complex frequency spectrum observed for an accreting Delta Scuti-type star (after Y Cam). In addition, we demonstrate that the amplitudes of several of these pulsation frequencies show evidence of variability on time scales as short as 1-2 years, perhaps even less. Moreover, our analysis takes into account some recently acquired spectra, from which we obtained the corresponding radial velocities for the years 2007-2009. Investigation of the O-C diagram shows that further monitoring of the epochs of eclipse minima of CT Her will cast a new light on the evolution of its orbital period.