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We present combined photometric and spectroscopic analyses of the southern binary star PU Pup. High-resolution spectra of this system were taken at the University of Canterbury Mt. John Observatory in the years 2008 and again in 2014-15. We find the light contribution of the secondary component to be only $sim$2% of the total light of the system in optical wavelengths, resulting in a single-lined spectroscopic binary. Recent TESS data revealed grazing eclipses within the light minima, though the tidal distortion, examined also from HIPPARCOS data, remains the predominating light curve effect. Our model shows PU Pup to have the more massive primary relatively close to filling its Roche lobe. PU Pup is thus approaching the rare `fast phase of interactive (Case B) evolution. Our adopted absolute parameters are as follows: $M_1$ = 4.10 ($pm$0.20) M$_{odot}$, $M_2$ = 0.65 ($pm$0.05) M$_{odot}$, $R_{1}$ = 6.60 ($pm$0.30) R$_{odot}$, $R_2$ = 0.90 ($pm$0.10) R$_{odot}$; $T_{1}$ = 11500 ($pm$500) K, $T_{2}$ = 5000 ($pm$350) K; photometric distance = 186 ($pm$20) pc, age = 170 ($pm$20) My. The less-massive secondary component is found to be significantly oversized and overluminous compared to standard Main Sequence models. We discuss this discrepancy referring to heating from the reflection effect.
New spectrometric data on V Pup are combined with satellite photometry (HIPPARCOS and recent TESS) to allow a revision of the absolute parameters with increased precision. We find: $M_1$ = 14.0$pm$0.5, $M_2$ = 7.3$pm$0.3 (M$_odot$); $R_{1}$ = 5.48$pm
We constructed a Hubble Space Telescope (HST) astro-photometric catalog of the central region of the Galactic globular cluster NGC 1261. This catalog, complemented with Gaia DR2 data sampling the external regions, has been used to estimate the struct
The photometric and spectroscopic data for three double-lined detached eclipsing binaries were collected from the photometric and spectral surveys. The light and radial velocity curves of each binary system were simultaneously analyzed by using Wilso
High-resolution spectroscopy is a powerful tool to study the dynamical structure of pulsating stars atmosphere. We aim at comparing the line asymmetry and velocity of the two delta Sct stars rho Pup and DX Cet with previous spectroscopic data obtaine
We report the results of a long-term spectroscopic monitoring of the A-type supergiant with the B[e] phenomenon 3 Pup = HD 62623. We confirm earlier findings that it is a binary system. The orbital parameters were derived using cross-correlation of t