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Context. The instability strip (IS) of classical Cepheids has been extensively studied theoretically. Comparing the theoretical IS edges with those obtained empirically, using the most recent Cepheids catalogs available, can provide us with insights into the physical processes that determine the position of the IS boundaries. Aims. We aim to investigate the empirical positions of the IS of the classical Cepheids in the Large Magellanic Cloud (LMC), considering any effect that increases its width, to obtain intrinsic edges that can be compared with theoretical models. Methods. We used data of classical fundamental-mode (F) and first-overtone (1O) LMC Cepheids from the OGLE-IV variable star catalog, together with a recent high-resolution reddening map from the literature. Our final sample includes 2058 F and 1387 1O Cepheids. We studied their position on the Hertzsprung-Russell diagram and determined the IS borders by tracing the edges of the color distribution along the strip. Results. We obtained the blue and red edges of the IS in V- and I-photometric bands, in addition to log Teff and log L. The results obtained show a break located at the Cepheids' period of about three days, which was not reported before. We compared our empirical borders with theoretical ones published in the literature, obtaining a good agreement for specific parameter sets. Conclusions. The break in the IS borders is most likely explained by the depopulation of second- and third-crossing classical Cepheids in the faint part of the IS, since blue loops of evolutionary tracks in this mass range do not extend blueward enough to cross the IS at the LMC metallicity. Results from the comparison of our empirical borders with theoretical ones prove that our empirical IS is a useful tool for constraining theoretical models. [ABSTRACT FROM AUTHOR]

We present non-linear hydrodynamic pulsation models for OGLE-BLG-RRLYR-02792 – a 0.26 M⊙ pulsator, component of the eclipsing binary system, analysed recently by Pietrzyński et al. The star’s light and radial velocity curves mimic that of classical RR Lyrae stars, except for the bump in the middle of the ascending branch of the radial velocity curve. We show that the bump is caused by the 2:1 resonance between the fundamental mode and the second overtone – the same mechanism that causes the Hertzsprung bump progression in classical Cepheids. The models allow us to constrain the parameters of the star, in particular to estimate its absolute luminosity (≈33 L⊙) and effective temperature (≈6970 K, close to the blue edge of the instability strip).We conduct a model survey for the new class of low-mass pulsators similar to OGLE-BLG-RRLYR-02792 – products of evolution in the binary systems. We compute a grid of models with masses corresponding to half (or less) of the typical mass of RR Lyrae variable, 0.20 ≤ M ≤ 0.30 M⊙, and discuss the properties of the resulting light and radial velocity curves. Resonant bump progression is clear and may be used to distinguish such stars from classical RR Lyrae stars. We present the Fourier decomposition parameters for the modelled light and radial velocity curves. The expected values of the φ31 Fourier phase for the light curves differ significantly from that observed in RR Lyrae stars, which is another discriminant of the new class. [ABSTRACT FROM AUTHOR]

Context. The Baade-Wesselink (BW) method of distance determination of Cepheids is used to calibrate the distance scale. Various versions of this method are mainly based on interferometry and/or the surface-brightness color relation (SBCR). Aims. We quantify the impact of the SBCR, its slope, and its zero point on the projection factor. This quantity is used to convert the pulsation velocity into the radial velocity in the BW method. We also study the impact of extinction and of a potential circumstellar environment on the projection factor. Methods. We analyzed HARPS-N spectra of η Aql to derive its radial velocity curve using different methods. We then applied the inverse BW method using various SBCRs in the literature in order to derive the BW projection factor. Results. We find that the choice of the SBCR is critical: a scatter of about 8% is found in the projection factor for different SBCRs in the literature. The uncertainty on the coefficients of the SBCR affects the statistical precision of the projection factor only little (1–2%). Confirming previous studies, we find that the method with which the radial velocity curve is derived is also critical, with a potential difference on the projection factor of 9%. An increase of 0.1 in E(B − V) translates into a decrease in the projection factor of 3%. A 0.1 mag effect of a circumstellar envelope (CSE) in the visible domain is rather small on the projection factor, about 1.5%. However, we find that a 0.1 mag infrared excess in the K band due to a CSE can increase the projection factor by about 6%. Conclusions. The impact of the surface-brightness color relation on the BW projection factor is found to be critical. Efforts should be devoted in the future to improve the SBCR of Cepheids empirically, but also theoretically, taking their CSE into account as well. [ABSTRACT FROM AUTHOR]

We report results from a search for Galactic high-mass eclipsing binaries. The photometric monitoring campaign was performed in Sloan r and i with the robotic twin refractor RoBoTT at the Universitätssternwarte Bochum in Chile and complemented by Johnson UBV data. Comparison with the SIMBAD data base reveals 260 variable high-mass stars. Based on well-sampled light curves, we discovered 35 new eclipsing high-mass systems and confirm the properties of six previously known systems. For all objects, we provide the first light curves and determine orbital periods through the Lafler–Kinman algorithm. Apart from GSC 08173-0018 and Pismis 24-13 (⁠|$P = 19.47\, d$| and |$20.14\, d$|⁠) and the exceptional short-period system TYC 6561-1765-1 (⁠|$P = 0.71\, d$|⁠), all systems have orbital periods between 1 and 9 d. We model the light curves of 26 systems within the framework of the Roche geometry and calculate fundamental parameters for each system component. The Roche lobe analysis indicates that 14 systems have a detached geometry, while 12 systems have a semidetached geometry; seven of them are near-contact systems. The deduced mass ratios q  = M 2/ M 1 reach from 0.4 to 1.0 with an average value of 0.8. The similarity of masses suggests that these high-mass binaries were created during the star formation process rather than by tidal capture. [ABSTRACT FROM AUTHOR]

We present the analysis of Blazhko-type modulation in double-mode RR Lyrae (RRd) stars found in the Optical Gravitational Lensing Experiment (OGLE) photometry of the Galactic bulge. Modulation is detected in 15 stars. Most of them have non-typical period ratio of the radial modes. In the Petersen diagram, at a given period of the fundamental mode, they are located significantly below or above the sequence formed by the majority of RRd stars. Multiperiodic modulation is very frequent; two or three modulation periods are detected in eight stars. Modulation periods vary from ∼20 to more than 300 d. Radial mode amplitudes can be modulated by a few to nearly 100 per cent. Both radial modes may be modulated with the same period. More commonly however, dominant modulation for the fundamental mode has different period than dominant modulation for the first overtone. Quite often modulation of only one mode is detected in the data. We find a clear feedback between pulsation amplitude of the dominant mode and mean stellar brightness: the lower the pulsation amplitude, the brighter the star. At phases of low pulsation amplitude, the mode periods are prone to fast changes. All the stars share the common feature: their pulsation properties are non-stationary. Amplitudes and phases of the radial modes vary irregularly on a long time-scale of a few hundred or thousand days. The short-term modulations are also irregular. One of the stars has switched the pulsation mode recently: from single-mode fundamental mode pulsation to RRd state. In other star the non-radial mode with characteristic ∼0.61 period ratio to the first overtone is detected. This non-radial mode is likely modulated with the same period as the radial modes. [ABSTRACT FROM AUTHOR]

Aims. High-resolution imaging in several photometric bands can provide color and astrometric information of the wide-orbit component of Cepheid stars. Such measurements are needed to understand the age and evolution of pulsating stars. In addition, binary Cepheids have the potential to provide direct and model-independent distances and masses. Methods. We used the NAOS-CONICA adaptive optics instrument (NACO) in the near-infrared to perform a deep search for wide components around the classical Cepheids, Y Oph, FF Aql, X Sgr,WSgr, and η Aql, within a field of view of 1.7" × 1.7" (3.4" × 3.4" for Aql). Results. We were able to reach contrast ΔH = 5-8 mag and ΔKs = 4-7 mag in the radius range r > 0.2", which enabled us to constrain the presence of wide companions. For Y Oph, FF Aql, X Sgr, W Sgr, and Aql at r > 0.2", we ruled out the presence of companions with a spectral type that is earlier than a B7V, A9V, A9V, A1V, and G5V star, respectively. For 0.1" < r < 0.2", no companions earlier than O9V, B3V, B4V, B2V, and B2V star, respectively, are detected. A component is detected close to Aql at projected separation ρ= 654.7 ± 0.9 mas and a position angle PA = 92.8 ± 0.1. We estimated its dereddened apparent magnitude to be mH0 = 9.34 ± 0.04 and derived a spectral type that ranges between an F1V and an F6V star. Additional photometric and astrometric measurements are necessary to better constrain this star and check its physical association to the η Aql system. [ABSTRACT FROM AUTHOR]

We present a variability study of 4646 massive stars in the Small Magellanic Cloud (SMC) with known spectral types from the catalog of Bonanos et al. (2010) using the light curves from the OGLE-III database. The goal is to exploit the time domain information available through OGLE-III to gain insight into the processes that govern the evolution of massive stars. This variability survey of massive stars with known spectral types is larger than any previous survey by a factor of 7. We find that 60% of our sample (2766 stars) show no significant variability and 40% (1880 stars) exhibit variability distributed as follows: 807 stars display low-amplitude stochastic variability with fluctuations in the I-band of up to 0.05 mag, 443 stars present irregular variability of higher amplitude (76% of these are reported as variables for the first time), 205 are eclipsing binaries (including 101 newly discovered systems), 50 are candidate rotating variables, 126 are classical Cepheids, 188 stars exhibit short-term sinusoidal periodicity (P < 3 days) making them candidate "slowly pulsating B stars" and non-radial Be pulsators, and 61 periodic stars exhibit longer periods. We demonstrate the wealth of information provided in the time domain, by doubling the number of known massive eclipsing binary systems and identifying 189 new candidate early-type Be and 20 Oe stars in the SMC. In addition, we find that ~80% of Be stars are photometrically variable in the OGLE-III time domain and provide evidence that short-term pulsating stars with additional photometric variability are rotating close to their break-up velocity. [ABSTRACT FROM AUTHOR]

ABSTRACT We report the discovery of a period doubling behaviour in a 2.4-d BL Herculis type variable of the Galactic bulge. Another bulge BL Her type star ( P = 2.25 d) is a strong period doubling candidate. Both objects have been identified with the Optical Gravitational Lensing Experiment (OGLE) photometry. Possibility of period doubling in this type of pulsators has been predicted almost 20 yr ago by Buchler & Moskalik. Our finding is the first observational confirmation of their theoretical results. Discovery of the first BL Herculis star showing the period doubling effect motivates a new theoretical investigation with the state-of-the-art convective pulsation codes. We present the results of initial model survey, specifically aimed at studying the observed period-doubled BL Her variable. All of our non-linear models have P = 2.4 d. The computations confirm that the period doubling effect is caused by the 3:2 resonance between the fundamental mode and the first overtone, as indicated by earlier radiative models of Buchler & Moskalik. Comparison of the computed and the observed light curves allows us to constrain the parameters of the star, in particular its metallicity, which appears to be high, Z ≈ 0.01. The recent evolutionary tracks put also constraint on the mass of the star, which is close to M = 0.50 M⊙. [ABSTRACT FROM AUTHOR]

We present the first spectroscopic data for a sample of the recently discovered blue double-periodic variables in the Magellanic Clouds. The optical spectrum of these objects is dominated by Balmer and helium absorption lines and a continuum with a blue or sometimes flat slope. Spectral classification yields B spectral types and luminosity classes mostly of type III. However, the Hβ absorption line is weaker than expected for the spectral classification in most objects. For two objects, OGLE 05060009-6855025 and OGLE 05195898-6917013 we obtained time-resolved spectroscopy, finding radial velocity variations consistent with binarity. Phasing the short-term photometric variability of these two systems with their spectroscopic ephemeris, we find that they can be interpreted as ellipsoidal variations of the brighter component in a close binary system. From the analysis of their short-term light curves and radial velocities, we estimate that the cooler component could be a B-type dwarf. Our findings support the hypothesis that double-periodic variables are close binary systems consisting of two B-type stars. The shorter periodicity in non-eclipsing systems should be the ellipsoidal variation of the more evolved component. Regarding the long-term periodicity, we find their origin in or around the brighter star, as the oscillations virtually disappear at primary eclipse. Their nature remains unknown, at the present time. We also report the discovery of three (two of them eclipsing) new double-periodic variables in the Large Magellanic Cloud. One of them shows a shortening of the long-term period by approximately 20 per cent in a couple of cycles, which coincides with an increase of the maximum oscillation brightness. [ABSTRACT FROM AUTHOR]