Key points are not available for this paper at this time.
Pulsating stars in eclipsing binary systems offer a unique possibility to empirically identify pulsation modes using the geometric effect of the eclipses on the pulsation signals. Here we explore the Scuti type pulsations in the eclipsing binary system KIC~3858884 with the aim of identifying the dominant modes using various photometric methods. We used the Kepler short cadence photometry data. Refined binary model and pulsation parameters were determined using an iterative separation of the eclipsing binary and pulsation signals. We used various methods to identify the host stars of the dominant pulsations. \'Echelle diagram diagnostics were employed to locate the frequencies with most influence from the eclipses. Direct Fitting methods assuming spherical harmonic surface patterns were explored to determine an orientation for the symmetry axis and to infer surface mode numbers and m. General surface patterns were reconstructed using dynamic eclipse mapping, and provided ancillary mode number estimates. We established the secondary star as the main source of the pulsations. Seven peaks, including the two strongest modes, were found to show modulations during the secondary eclipses. For the first time ever, we could detect two hidden modes with amplitude intensification during the eclipses. Only one frequency appears to originate from the primary. We successfully reconstructed surface patterns and determined mode numbers for most of the selected frequencies with both of our methods. One radial and three sectoral modes, among them hidden modes. The two hidden modes were identified as (3, 1) and (2, 1). One additional radial mode turned out to be a combination frequency. Partial disagreement between EM and DF results may indicate that the strongest modes deviate from strict spherical harmonics.
Bókon et al. (Mon,) studied this question.