Massive pulsating stars observed by BRITE-Constellation. I. The triple system Beta Centauri (Agena)

TL;DR

This study uses BRITE-Constellation photometry to precisely determine the masses and pulsation modes of the massive components of Beta Centauri, revealing complex oscillation spectra and potential hybrid pulsations in a rapidly rotating star.

Contribution

It provides the first detailed seismic analysis of Beta Centauri's components, including mass measurements and mode identification, demonstrating the capabilities of BRITE data for massive pulsating stars.

Findings

Masses of components: 12.02 and 10.58 solar masses

Detected 19 pulsation terms, including g and p modes

Potential hybrid Beta Cep/SPB pulsators

Abstract

This paper aims to precisely determine the masses and detect pulsation modes in the two massive components of Beta Cen with BRITE-Constellation photometry. In addition, seismic models for the components are considered and the effects of fast rotation are discussed. This is done to test the limitations of seismic modeling for this very difficult case. A simultaneous fit of visual and spectroscopic orbits is used to self-consistently derive the orbital parameters, and subsequently the masses, of the components. The derived masses are equal to 12.02 +/- 0.13 and 10.58 +/- 0.18 M_Sun. The parameters of the wider, A - B system, presently approaching periastron passage, are constrained. Analysis of the combined blue- and red-filter BRITE-Constellation photometric data of the system revealed the presence of 19 periodic terms, of which eight are likely g modes, nine are p modes, and the remaining two are combination terms. It cannot be excluded that one or two low-frequency terms are rotational frequencies. It is possible that both components of Beta Cen are Beta Cep/SPB hybrids. An attempt to use the apparent changes of frequency to distinguish which modes originate in which component did not succeed, but there is potential for using this method when more BRITE data become available. Agena seems to be one of very few rapidly rotating massive objects with rich p- and g-mode spectra, and precisely known masses. It can therefore be used to gain a better understanding of the excitation of pulsations in relatively rapidly rotating stars and their seismic modeling. Finally, this case illustrates the potential of BRITE-Constellation data for the detection of rich-frequency spectra of small-amplitude modes in massive pulsating stars.