- ID:
- ivo://CDS.VizieR/J/A+A/578/A136
- Title:
- Period changes in SuperWASP eclipsing binaries
- Short Name:
- J/A+A/578/A136
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Orbital period changes of binary stars may be caused by the presence of a third massive body in the system. Here we have searched the archive of the Wide Angle Search for Planets (SuperWASP) project for evidence of period variations in 13927 eclipsing binary candidates. Sinusoidal period changes, strongly suggestive of third bodies, were detected in 2% of cases; however, linear period changes were observed in a further 22% of systems. We argue on distributional grounds that the majority of these apparently linear changes are likely to reflect longer-term sinusoidal period variations caused by third bodies, and thus estimate a higher-order multiplicity fraction of 24% for SuperWASP binaries, in good agreement with other recent figures for the fraction of triple systems amongst binary stars in general.
Number of results to display per page
Search Results
- ID:
- ivo://CDS.VizieR/J/MNRAS/405/1930
- Title:
- Period changes of EA-, EB- and EW-types binaries
- Short Name:
- J/MNRAS/405/1930
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Cyclic period changes are a fairly common phenomenon in close binary systems and are usually explained as being caused either by the magnetic activity of one or both components or by the light travel time effect (LTTE) of a third body. We searched the orbital period changes in 182 EA-type (including the 101 Algol systems used by Hall, 1989, Space Sci. Rev., 50, 219), 43 EB-type and 53 EW-type binaries with known mass ratio and spectral type of the secondary component. We reproduced and improved the diagram in Hall according to the new collected data.
- ID:
- ivo://CDS.VizieR/J/AcA/56/253
- Title:
- Period changes of OGLE contact binaries
- Short Name:
- J/AcA/56/253
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Presented are results of determination of secular period changes for 569 contact binaries from the OGLE database with periods shorter than about one day and observations spanning 14 observing seasons. The statistically significant rates of secular changes found for 134 stars are distributed nearly symmetrically around zero with a half-width of the distribution equal to about 3.5x10^-7^d/yr. The remaining rates are confined within the error distribution with dispersion about 2.3x10^-7^d/yr. The largest rates of period change that have been found are of the order of 5x10^-6^d/yr.
- ID:
- ivo://CDS.VizieR/J/ApJ/773/1
- Title:
- Period of HD 19356 recorded in the Cairo Calendar?
- Short Name:
- J/ApJ/773/1
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The eclipses in binary stars give precise information of orbital period changes. Goodricke J. (1783RSPT...73..474G) discovered the 2.867d period in the eclipses of Algol. The irregular orbital period changes of this longest known eclipsing binary continue to puzzle astronomers. The mass transfer between the two members of this binary should cause a long-term increase of the orbital period, but observations over two centuries have not confirmed this effect. Here, we present evidence indicating that the period of Algol was 2.850d three millennia ago. For religious reasons, the ancient Egyptians have recorded this period into the Cairo Calendar (CC), which describes the repetitive changes of the Raging one. CC may be the oldest preserved historical document of the discovery of a variable star.
- ID:
- ivo://CDS.VizieR/J/A+A/602/A117
- Title:
- Periods of 2290 CoRoT binaries
- Short Name:
- J/A+A/602/A117
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The CoRoT mission during its flight-phase 2007-2012 delivered the light-curves for over 2000 eclipsing binaries. Data from the Kepler mission have proven the existence of several transiting circumbinary planets. Albeit light-curves from CoRoT have typically lower precision and shorter coverage, CoRoT's number of targets is similar to Kepler, and some of the known circumbinary planets could potentially be detected in CoRoT data as well. The aim of this work has been a revision of the entire CoRoT data-set for the presence of circumbinary planets, and the derivation of limits to the abundances of such planets. We developed a code which removes the light curve of the eclipsing binaries and searches for quasi-periodic transit-like features in a light curve after removal of binary eclipses and instrumental features. The code needs little information on the sample systems and can be used for other space missions as well, like Kepler, K2, TESS and PLATO. The code is broad in the requirements leading to detections, but was tuned to deliver an amount of detections that is manageable in a subsequent, mainly visual, revision about their nature. In the CoRoT sample we identified three planet candidates whose transits would have arisen from a single pass across the central binary. No candidates remained however with transit events from multiple planetary orbits. We calculated the upper limits for the number of Jupiter, Saturn and Neptune sized planets in co-planar orbits for different orbital period ranges. We found that there are much less giant planets in short-periodic orbits around close binary systems than around single stars.
- ID:
- ivo://CDS.VizieR/J/A+A/489/321
- Title:
- Period study of TW Draconis
- Short Name:
- J/A+A/489/321
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a study of time series data for the Algol-type eclipsing binaries TW Draconis obtained over the past 150 years to detect changes in minima timings. There is significant evidence for miscellaneous interacting physical processes in the system, which manifest themselves as for example period and light curve changes. Using 561 available minima timings, we compile an extended O-C diagram analysis. A detailed description of period changes allows us to construct the true phased light curve at any moment. The timing residuals (according to the linear ephemeris) display two stages of differing behaviour in 1858-2007. The first part ends around 1942. It is characterized by more or less smooth linear/parabolic course of timing residuals. In 1858-1905, the period was almost constant P=2.806513(9)d, but, in 1905-1942, the period increased due to mass exchange between components. Since 1942, the system has been showing alternating and shortening period changes with the length of a cycle of about two decades, modulated by short-term periodic variations. The latter small variations with the period 6.5-years are caused by the light-time effect due to the presence of a third low-mass body in the system. Major oscillations can be explained as consequences of quadrupole moment variation in the system.
- ID:
- ivo://CDS.VizieR/J/A+A/566/A128
- Title:
- Period variations in SuperWASP PCEB
- Short Name:
- J/A+A/566/A128
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Period or amplitude variations in eclipsing binaries may reveal the presence of additional massive bodies in the system, such as circumbinary planets. Here, we have studied twelve previously-known eclipsing post-common-envelope binaries for evidence of such light curve variations, on the basis of multi-year observations in the SuperWASP archive. The results for HW Vir provided strong evidence for period changes consistent with those measured by previous studies, and help support a two-planet model for the system. ASAS J102322-3737.0 exhibited plausible evidence for a period increase not previously suggested; while NY Vir, QS Vir and NSVS 14256825 afforded less significant support for period change, providing some confirmation to earlier claims. In other cases, period change was not convincingly observed; for AA Dor and NSVS 07826147, previous findings of constant period were confirmed. This study allows us to present hundreds of new primary eclipse timings for these systems, and further demonstrates the value of wide-field high-cadence surveys like SuperWASP for the investigation of variable stars.
- ID:
- ivo://CDS.VizieR/J/PASP/108/332
- Title:
- Photometric analysis of contact binaries
- Short Name:
- J/PASP/108/332
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present BV light-curve synthetic analyses of three short-period contact (W UMa) binaries: HY Pavonis (P=~0.35days), AW Virginis (P=~0.35days), and BP Velorum (P=~0.26days). Different possible configurations for wide range of the mass ratio were explored in each case making use of the Wilson-Devinney code. The photometric parameters of the systems were determined from the synthetic light-curve solutions that best fit the observations. AW Vir has two components of very similar temperatures and therefore the subtype (A or W) remains undetermined. HY Pav and BP Vel are best modeled by W-type configurations and the asymmetries in the light curves are reproduced by introducing cool spots on the more massive secondary components. Although BP Vel lies in the region of the open cluster Cr 173, its distance modulus, in principle, rules it out as a cluster member.
- ID:
- ivo://CDS.VizieR/J/AJ/143/129
- Title:
- Photometric and Spectroscopic observations of BF Dra
- Short Name:
- J/AJ/143/129
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- BF Dra is now known to be an eccentric double-lined F6+F6 binary star with relatively deep (0.7mag) partial eclipses. Previous studies of the system are improved with 7494 differential photometric observations from the URSA WebScope and 9700 from the NFO WebScope, 106 high-resolution spectroscopic observations from the Tennessee State University 2m automatic spectroscopic telescope and the 1m coude-feed spectrometer at Kitt Peak National Observatory, and 31 accurate radial velocities from the CfA. Very accurate (better than 0.6%) masses and radii are determined from analysis of the two new light curves and four radial velocity curves. Theoretical models match the absolute properties of the stars at an age of about 2.72Gyr and [Fe/H]=-0.17, and tidal theory correctly confirms that the orbit should still be eccentric. Our observations of BF Dra constrain the convective core overshooting parameter to be larger than about 0.13H_p_. We find, however, that standard tidal theory is unable to match the observed slow rotation rates of the components' surface layers.
- ID:
- ivo://CDS.VizieR/J/AJ/158/193
- Title:
- Photometric data of V582 Lyr and V1016 Oph
- Short Name:
- J/AJ/158/193
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present new CCD photometric light curves about two eclipsing binaries of V582 Lyr and V1016 Oph. Our observations were carried out by the SARA 91.4 cm telescope of America in 2016 and the 60 cm telescope of Chile in 2018. V582 Lyr's spectra type was classified as K5, and its radial velocity was determined using the LAMOST spectral survey. There are absorptions in the observed H{alpha} line and excess emissions in the subtracted H{alpha} line, which show weak chromospheric activity. We obtained the updated ephemeris information for V582 Lr and V1016 Oph, and found that their orbital periods are both decreasing. We concluded that the decreased rate is -0.474 (+/-0.011)x10^-7^ days/yr for V582 Lyr and 3.460 (+/-0.014)x10^-7^ days/yr for V1016 Oph. For V582 Lyr, the period variation was interpreted as a mass transfer from the secondary component to the primary one, and the corresponding rate is dM_2_/dt=-1.10 (+/-0.03)x10^-7^ M_{sun}_/yr. For V1016 Oph, we explain it by transferring from the primary component to the secondary one, and the corresponding rate is dM_1_/dt=-2.69 (+/-0.04)x10^-7^ M_{sun}_/yr. The photometric solution of V1016 Oph was obtained by analyzing the CCD photometry with the Wilson-Devinney program. We also obtained the orbital parameters of V1016 Oph by simultaneously analyzing our BVRI light curves and radial-velocity curve from the LAMOST low-resolution spectral survey. Finally, our orbital solution shows that they are contact eclipsing binaries with contact factors of 3.35 (+/-0.08)% for V582 Lyr and 41.0 (+/-0.1)% for V1016 Oph.
