MOST light-curve analysis of the gamma Dor pulsator HR 8799, showing resonances and amplitude variations

TL;DR

This study analyzes the pulsation properties of the gamma Doradus star HR 8799 using nearly continuous 47-day photometry from the MOST space telescope, revealing resonance phenomena and amplitude variations that complicate asteroseismic modeling.

Contribution

It provides detailed Fourier analysis of HR 8799's pulsations, identifying multiple frequency multiples and amplitude variations, advancing understanding of its pulsation behavior.

Findings

Resonance and amplitude changes characterize HR 8799's pulsations.

Dominant frequency at 1.978 c/d with multiples at n/9 f1.

Amplitude and phase variations occur on a 47-day timescale.

Abstract

Context: The central star of the HR 8799 system is a gamma Doradus-type pulsator. The system harbours four planetary-mass companions detected by direct imaging, and is a good solar system analogue. The masses of the companions are not known accurately, because the estimation depends strongly on the age of the system, which is also not known with sufficient accuracy. Asteroseismic studies of the star might help to better constrain the age of HR 8799. We organized an extensive photometric and multi-site spectroscopic observing campaign for studying the pulsations of the central star. Aims: The aim of the present study is to investigate the pulsation properties of HR 8799 in detail via the ultra-precise 47-d-long nearly continuous photometry obtained with the MOST space telescope, and to find as many independent pulsation modes as possible, which is the prerequisite of an asteroseismic age determination. Methods: We carried out Fourier analysis of the wide-band photometric time series. Results: We find that resonance and sudden amplitude changes characterize the pulsation of HR 8799. The dominant frequency is always at f1 = 1.978 c/d. Many multiples of one ninth of the dominant frequency appear in the Fourier spectrum of the MOST data: n/9 f1, where n={1, 2, 3, 4, 5, 6, 7, 8, 9, 10, 13, 14, 17, 18}. Our analysis also reveals that many of these peaks show strong amplitude decrease and phase variations even on the 47-d time-scale. The dependencies between the pulsation frequencies of HR 8799 make the planned subsequent asteroseismic analysis rather difficult. We point out some resemblance between the light curve of HR 8799 and the modulated pulsation light curves of Blazhko RR Lyrae stars.