Anya SamadiALMA-Conicyt Postdoctoral fellow
Academic degreePhD University of Tabriz, Iran (2011-2018) - Thesis title: The Pulsation Study and Light curve Analyses Of Some Kepler γ Doradus(/δ Scuti) Eclipsing Binary Stars (distinction)
Telephone56 (2) 221-38159
In my research I mainly care about Binary stars. I call them “El Dorado” of the Astrophysics. Binary stars are perfect laboratories to test crucial astrophysical studies (eccentricity, tidal effects, mass transfer, chemical peculiarities, presence of a third body, etc.). Most significantly, we need them to derive the stellar masses with high precision. Double-lined spectroscopic binaries, eclipsing binaries (EBs) together with stellar models can give us the accurate radius and masses of stars with 1-2% precision. In the era of large spectro-photometric surveys like Gaia, we can access parallaxes, absolute magnitudes, and luminosities of a large population of binary stars that, at the end, having their ages let us decode the stellar evolution stories. The recent challenge for me is to answer how precise the stellar parallaxes are for the binary systems! Unprecedented photometric observation from space missions like Kepler, K2 and TESS has provided us with stellar masses from "Asteroseismology". About 14% of main-sequence intermediate-mass (A/F-type) stars in the binary systems are gamma Dor/delta Scuti pulsators; many of the subgroups of which are thew fast rotators (vsini >70 Km/s). Studying the hybrid binary stars, with both gamma Dor/ delta Scuti pulsations, and fast-rotation provides both precise stellar parameters and the fingerprints of how binarity and rotation can influence the stellar pulsation, structure, and evolution.
Binary stars (SB2/EBs);
Stellar pulsations in A/F-type binary stars (Hybrid, γ Doradus/δ Scuti pulsations);
Distance measurements for binary stars
See recent key paper HERE. Here, I have used the photometric data (light curves) from Kepler space mission along with Fourier spectrum of a SB2 system to detect stellar pulsations modes that are excited close to core (gravity modes), close to surface (acoustic modes) and another group of low-frequency modes that are excited because of the Stella fast-rotation rotation (Rossby modes).