LIGHT CURVES AND FREQUENCY ANALYSIS OF HYBRID  SCT- DOR STARS

Abstract

Space observations have greatly improved our knowledge of stellar oscillations since they allowed us to discover many oscillation frequencies with small amplitudes that used to be hidden from the ground observations. One of the interesting phenomena revealed was a large number of hybrid Sct- Dor stars discovered. These objects are low-mass main sequence stars oscillating in
radial and non-radial pressure (p) and gravity (g) modes. The simultaneous presence of p- and g- modes in these stars makes them excellent targets for asteroseismology since these modes together allow to probe both the external and near-to-core layers of the stars. Nevertheless, their location at the Hertzsprung-Russel diagram indicates they might have surface activity (spots) hindering the correct classification of oscillation modes in the frequency spectrum, especially at low-frequency ranges. Additionally, these objects might be in binary systems, which makes mode classification, and thus the explanation of the origin of their light curve variability, an even more complex task. In this work, we present a frequency analysis of the hybrid Sct- Dor star CoRoT-102314644 and summarize the difficulties that arise when classifying the origin of the light curve variations in this type of objects.