- ID:
- ivo://CDS.VizieR/J/AJ/139/2347
- Title:
- CO And Vr light curves and RV curve
- Short Name:
- J/AJ/139/2347
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Accurate absolute properties have been determined for the eclipsing triple star CO And (F8+F8) based on extensive differential photometry obtained by three robotic observatories and CfA spectroscopy. The eclipsing binary star orbit is circular with a period of 3.655days. The triple nature of this system is revealed by more than a century of timings of minimum light, and by the presence of third light in the photometric orbits.
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- ID:
- ivo://CDS.VizieR/J/AJ/146/123
- Title:
- Coefficients in JHKs for the Wilson-Devinney code
- Short Name:
- J/AJ/146/123
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In this paper, radial velocity and VI- and JHKs (Two Micron All Sky Survey) band photometric data of the detached system HV Cnc have been analyzed. The primary component of HV Cnc, which is a member of the M67 cluster, is suspected to be either a blue straggler or turn-off star. The system is a single-lined spectroscopic binary and its light curve shows a total eclipse. Spectroscopic observations of the system revealed the third component, which shows contribution to the total light of the system. Light curve and radial velocity data have been analyzed using the Wilson-Devinney (W-D) code and JHKs filter definitions computed for the W-D code in this work. Our analysis shows that the mass and radius of the primary and secondary components are 1.31M_{sun}_, 0.52M_{sun}_, 1.87R_{sun}_, and 0.48R_{sun}_, respectively. All results are compared with previously published literature values and discussed.
- ID:
- ivo://CDS.VizieR/J/ApJS/254/10
- Title:
- Compilation of W UMa stars
- Short Name:
- J/ApJS/254/10
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a statistical study of the largest bibliographic compilation of stellar and orbital parameters of W UMa stars derived by light-curve synthesis with Roche models. The compilation includes nearly 700 individually investigated objects from over 450 distinct publications. Almost 70% of this sample is comprised of stars observed in the past decade that have not been considered in previous statistical studies. We estimate the ages of the cataloged stars, model the distributions of their periods, mass ratios, temperatures, and other quantities, and compare them with the data from the Catalina Real-Time Transient Survey, LAMOST, and Gaia archives. As only a small fraction of the sample has radial-velocity curves, we examine the reliability of the photometric mass ratios in totally and partially eclipsing systems and find that totally eclipsing W UMa stars with photometric mass ratios have the same parameter distributions as those with spectroscopic mass ratios. Most of the stars with reliable parameters have mass ratios below 0.5 and orbital periods shorter than 0.5 days. Stars with longer periods and temperatures above 7000K stand out as outliers and should not be labeled W UMa binaries.
- ID:
- ivo://CDS.VizieR/J/MNRAS/465/4678
- Title:
- 9380 contact binaries from CRTS VSC
- Short Name:
- J/MNRAS/465/4678
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We construct a sample of 9380 contact binaries (W UMa systems) by using the Catalina Real-Time Transient Survey Variables Sources Catalogue. By measuring brightness change rates, light-curve statistics, and temperatures for this sample, we improve the understanding of contact binary light-curve characteristics, and luminosity variability on decadal time-scales. We show that binaries with convective outer envelopes have a different distribution of light-curve amplitudes and magnitude differences between eclipse minima than binaries with radiative outer envelopes. We find that more than 2000 binaries exhibit a linear change in mean brightness over the 8-yr timespan of observations with at least 3{sigma} significance. We note that 25.9 per cent of binaries with convective outer envelopes exhibit a significant change in brightness, while only 10.5 per cent of radiative binaries exhibit a significant change in brightness. In 205 binaries (2.2 per cent), we find that a sinusoid model better describes the luminosity trend within the 8-yr observation timespan. For these binaries, we report the amplitudes and periods (as estimated using observed half-periods) of this sinusoidal brightness variation and discuss possible mechanisms driving the variation.
- ID:
- ivo://CDS.VizieR/J/AcA/51/259
- Title:
- Contact binaries in OGLE-I database
- Short Name:
- J/AcA/51/259
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The present catalog contains the most numerous, observationally homogeneous sample of contact binaries. It is derived from the OGLE experiment (Optical Gravitational Lensing Experiment), in the direction of the Galactic Bulge and the Galactic bar. The observations were made with the 1-m Swope telescope at Las Campanas Observatory in Chile, over the period 1992 to 1995. The present catalog includes the 1575 newly discovered contact binaries fainter than I=18mag as well as the 1165 brighter contact binaries previously published. It also includes a list of 506 objects with nearly sinusoidal light curves, to ease the comparison and/or distinction between contact binaries with the sinusoidal light curves and pulsating stars.
- ID:
- ivo://CDS.VizieR/J/A+A/565/A55
- Title:
- CoRoT 105906206 frequencies analysis
- Short Name:
- J/A+A/565/A55
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Eclipsing binary systems with pulsating components allow determination of several physical parameters of the stars, such as mass and radius, that can be used to constrain the modeling of stellar interiors and evolution when combined with the pulsation properties. We present the results of the study of CoRoT 105906206, an eclipsing binary system with a pulsating component located in the CoRoT LRc02 field. The analysis of the CoRoT light curve was complemented by high-resolution spectra from the Sandiford at McDonald Observatory and FEROS at ESO spectrographs, which revealed a double-lined spectroscopic binary. We used an iterative procedure to separate the pulsation-induced photometric variations from the eclipse signals. First, a Fourier analysis was used to identify the significant frequencies and amplitudes due to pulsations. Second, after removing the contribution of the pulsations from the light curve we applied the PIKAIA genetic-algorithm approach to derive the best parameters for describing the system orbital properties.
- ID:
- ivo://CDS.VizieR/J/A+A/556/A87
- Title:
- CoRoT-100866999 frequency analysis
- Short Name:
- J/A+A/556/A87
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The presence of g- and p-modes allows testing stellar models from the core to the envelope. Moreover, binarity in an eclipsing system constrains the physical parameters of the pulsating star. CoRot ID 100866999 is a relatively large-amplitude hybrid gamma Doradus-delta Scuti star with two clearly distinct frequency domains. The large number of detected frequencies allows a detailed study of the interaction between them. In addition, we can derive the fundamental parameters of both components from the study of the eclipsing light curve. After removing the eclipsing phases, we analyzed the data with the Period04 package up to a signal-to-noise ratio S/N=4. The light curve was then prewhitened with these oscillation frequencies to derive the fundamental parameters of the two components.
- ID:
- ivo://CDS.VizieR/J/A+A/552/A60
- Title:
- CoRoT 102918586 light curve and spectra
- Short Name:
- J/A+A/552/A60
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Pulsating stars in eclipsing binary systems are powerful tools to test stellar models. Binarity enables us to constrain the pulsating component physical parameters and this knowledge drastically improves the input physics for asteroseismic studies. The study of stellar oscillations then allows us to improve our understanding of stellar interiors and stellar evolution. The space mission CoRoT discovered several promising objects suitable for these studies. They were photometrically observed with unprecedented accuracy, but needed spectroscopic follow-up. A promising target was the relatively bright eclipsing system CoRoT 102918586, which turned out to be a double-lined spectroscopic binary and also showed clear evidence of Gamma Dor type pulsations. With the aim of combining the information from binarity and pulsation and fully exploiting the potential of CoRoT photometry we obtained phase resolved high-resolution spectroscopy with the Sandiford spectrograph at the McDonald 2.1m telescope and the FEROS spectrograph at the ESO 2.2m telescope. Spectroscopy yielded both the radial velocity curves and, after spectra disentangling, the component effective temperatures, metallicity, and line-of-sight projected rotational velocities. The CoRoT light curve was analyzed with an iterative procedure, devised to disentangle eclipses from pulsations. The eclipsing binary light curve analysis, combined with the spectroscopic results, provided an accurate determination of the system parameters, and the comparison with evolutionary models provided strict constraints on the system age. Finally, the residuals obtained after subtraction of the best fitting eclipsing binary model were analyzed to determine the pulsator properties. We achieved a complete and consistent description of the system. The primary star pulsates with typical gamma Dor frequencies and shows a splitting in period that is consistent with high order g-mode pulsations in a star of the corresponding physical parameters. The value of the splitting, in particular, is consistent with pulsations in l=1 modes.
- ID:
- ivo://CDS.VizieR/J/A+A/597/A55
- Title:
- Corot photometry of TYC 455-791-1
- Short Name:
- J/A+A/597/A55
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery and analysis of very narrow transits in the eccentric spectroscopic binary TYC 455-791-1=HSS 348 (IC 4756). We obtained high-precision CoRoT photometry over two long runs and multi-epoch high-resolution echelle spectroscopy and imaging with STELLA. Standard radial-velocity extraction, spectrum synthesis, Fourier analysis, and light-curve inversions are applied to the data. HSS 348 is found to be an eccentric (e=0.18) double-lined spectroscopic binary with a period of 12.47 d in which at least the primary component is a peculiar B star of the HgMn class. The orbital elements are such that the system undergoes a grazing eclipse with the primary in front but no secondary eclipse. The out-of-eclipse light variations show four nearly equidistant but unequal minima stable in shape and amplitude throughout our observations. Their individual photometric periods are all harmonics of the same fundamental period which happens to agree with the transit period to within the errors. We interpret the fundamental period to be the rotation period of at least one if not both stars due to surface inhomogeneities. Due to the non-zero eccentricity of the orbit the two components are rotating sub-synchronously. It appears that HSS 348 is not a member of the IC 4756 cluster but a background B8+B8.5 binary system. Its sharp eclipses every 12.47 days just mimic a small-body transit but are in reality the grazing eclipses of a B-star binary and thus a classical false positive. The system seems to be pre-main sequence with the primary possibly just arrived on the ZAMS. The light curve with four unequal minima can be explained with four cool spots of different size equidistantly positioned in longitude. Our data do not allow to uniquely assign the spots to either of the two stars.
- ID:
- ivo://CDS.VizieR/J/MNRAS/454/2946
- Title:
- CSS detached eclipsing binaries
- Short Name:
- J/MNRAS/454/2946
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Eclipsing binaries play pivotal roles in our understanding of stellar properties. In the era of all-sky surveys, thousands of eclipsing binaries have been charted, yet their light curves remain unexplored. The goal of this work is to use time series and colour information to extract physical parameters of the binary systems when the spectroscopic information is not available. Inspired by the work of Devor et al., we use the Detached Eclipsing Binary Light curve fitter (DEBiL) and the Method for Eclipsing Component Identification (MECI) to derive basic properties of the binary systems identified by the Catalina Sky Surveys. We derive the mass, fractional radius, and age for 2170 binary systems. We report 211 eccentric systems and compare their properties to the tidal circularization theory. From the mass estimate, we present a subsample of low-mass M-dwarfs which warrant further follow-up to test the stellar models at the low-mass regime. With MECI, we are able to estimate the distance to individual eclipsing binary system and use them to probe the large-scale structure of the Milky Way. We demonstrate that DEBiL and MECI are instrumental to investigate eclipsing binary light curves in the era of all-sky surveys, and provide estimates of stellar parameters when the spectroscopic information is not available.
