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The main obstacle in exploiting the frequency data of $delta$ Sct stars is difficulty in mode identification. The $delta$ Sct oscillation spectra, unlike those of the Sun or white dwarfs, do not exhibit very regular patterns. Thus, the mode identification must rely on sophisticated methods, which involve combined multi-passband photometry and radial velocity data, with an unavoidable theoretical input from stellar atmosphere models. Moreover, there are serious uncertainties in theory of $delta$ Sct stars that have to be solved. Mode identification and determination of global and internal structure parameters for $delta$ Sct stars has to be done simultaneously. I describe in some detail the methodology and present some recent results we obtained concerning degrees of excited modes, global stellar parameters, and constraints on models of subphotospheric convection, as well as effect of rotational mode coupling.
The present paper provides a general overview of the asteroseismic potential of delta Scuti stars in clusters, in particular focusing on convection diagnostics. We give a summarise of the last results obtained by the authors for the Praesepe cluster
The current knowledge of the abundance pattern in delta Scuti stars is based on the analysis of just a few field stars. We aim to determine the general chemical properties of the atmospheres of delta Scuti stars based on a statistically relevant samp
Bi-site time-series photometric and high-resolution spectroscopic observations were made for the double-mode high-amplitude $delta$ Scuti star VX Hya. The fundamental frequency $f_{0}=4.4763 rm{c days^{-1}}$, the first overtone $f_{1}=5.7897 rm{c day
We present statistical characteristics of 1,578 {delta} Scuti stars including nearby field stars and cluster member stars within the Milky Way. We obtained 46% of these stars (718 stars) from the works done by Rodr{i}guez and collected the remaining
We have carried out a photometric and spectroscopic survey of bright high-amplitude delta Scuti (HADS) stars. The aim was to detect binarity and multiperiodicity (or both) in order to explore the possibility of combining binary star astrophysics with