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This paper aims to precisely determine the masses and detect pulsation modesin the two massive components of Beta Cen with BRITE-Constellation photometry.In addition, seismic models for the components are considered and the effectsof fast rotation are discussed. This is done to test the limitations of seismicmodeling for this very difficult case. A simultaneous fit of visual andspectroscopic orbits is used to self-consistently derive the orbitalparameters, and subsequently the masses, of the components. The derived massesare equal to 12.02 +/- 0.13 and 10.58 +/- 0.18 M_Sun. The parameters of thewider, A - B system, presently approaching periastron passage, are constrained.Analysis of the combined blue- and red-filter BRITE-Constellation photometricdata of the system revealed the presence of 19 periodic terms, of which eightare likely g modes, nine are p modes, and the remaining two are combinationterms. It cannot be excluded that one or two low-frequency terms are rotationalfrequencies. It is possible that both components of Beta Cen are Beta Cep/SPBhybrids. An attempt to use the apparent changes of frequency to distinguishwhich modes originate in which component did not succeed, but there ispotential for using this method when more BRITE data become available. Agenaseems to be one of very few rapidly rotating massive objects with rich p- andg-mode spectra, and precisely known masses. It can therefore be used to gain abetter understanding of the excitation of pulsations in relatively rapidlyrotating stars and their seismic modeling. Finally, this case illustrates thepotential of BRITE-Constellation data for the detection of rich-frequencyspectra of small-amplitude modes in massive pulsating stars.

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