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Delta Scuti stars are pulsating A- and F-type stars which, in principle have their internal structure and parameters including age, ascertained by their pulsation modes. Despite the vast amount of photometric data from space-based probes, observations are often still not matched with theoretical models. It remains uncertain if there are significant missing physics in the models, or if the observations are insufficient or inaccurate to explain these stellar objects. Two factors significantly contribute to this failure: accurate rotation rates and densities of the delta Sct stars. Both these parameters can be determined if the delta Sct star is a component of a binary system as I illustrate by the binaries, TT Hor and RZ Mic. Successful mode identification in both delta Sct components required higher than solar metallicity for evolutionary models suggesting some short comings in this procedure. In the future, the combination of the mode spectrum, Gaia distance and projected rotational velocity, may enable the application of work in this thesis to single stars. |
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