Discovery of the first octupole pulsation mode in a δ Scuti star

Aims. We attempt to understand better how stellar pulsations in close binary systems are affected, and possibly induced, by tidal, Coriolis, and centrifugal forces. Methods. We analyzed TESS data for some 50 000 potential eclipsing binaries selected by machine-learning algorithms in order to search for pulsation multiplets split by integer multiples of the orbital frequency. Results. We report the discovery of an octupole pulsation mode in the binary star system TIC 287869463. The star system contains a δ Scuti star. This mode is actually a combination of Y 3 + 3 and Y 3 − 3 modes that are perturbed into a new eigenmode of the star via tidal, Coriolis, and centrifugal forces, which we call a Y 33+ mode. The mode is stationary on the star, as opposed to being a traveling wave around the pulsation equator. To our knowledge, this is the first time that such an ℓ = 3 mode identification has been securely made in any δ Scuti star, and it is the first stationary ℓ = 3 sectoral mode of this type seen in any star, including the Sun. The ℓ = 3 pulsations appear as a combination of two components at 34.94617 d −1 and 39.31127 d −1 , split by exactly six times the frequency of the orbital motion to within better than 1 part in 10 5 . We extracted the pulsation frequencies from the TESS data spanning more than three years and modeled the system to gain a better understanding of this novel asteroseismic discovery. The pulsation frequencies are found to steadily increase with time, but they always maintain a split equal to six times the orbital frequency. Conclusions. We discuss the implications for the broader class of tidally tilted pulsators and triaxial pulsators that have been discovered to date. We conclude that these previous categories can all be interpreted as linear combinations of spherical harmonics whose axes coincide with the orbital axis and form new eigenmodes of the star via tidal, Coriolis, and centrifugal perturbations