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- ID:
- ivo://CDS.VizieR/J/AJ/114/326
- Title:
- MACHO Variables V.
- Short Name:
- J/AJ/114/326
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the characteristics of 611 eclipsing binary stars in the Large Magellanic Cloud found by using the MACHO Project photometry database. The sample is magnitude limited, and extends down the main sequence to about spectral type A0. Many evolved binaries are also included. Each eclipsing binary is classified according to the traditional scheme of the General Catalogue of Variable Stars (EA and EB), and also according to a new decimal classification scheme defined in this paper. The new scheme is sensitive to the two major sources of variance in eclipsing binary star light curves -- the sum of radii, and the surface-brightness ratio, and allow greater precision in characterizing the light curves. Examples of each type of light curve and their variations are given. Sixty-four of the eclipsing binaries have eccentric, rather than circular, orbits. The ephemeris and principal photometric characteristics of each eclipsing binary are listed in a table. Photometric orbits based on the Nelson-Davis-Etzel model have been fitted to all light curves. These data will be useful for planning future observations of these binaries. Plots of all data and fitted orbits and a table of the fitted orbital parameters are available on the AAS CD-ROM series, Vol. 9, 1997. These data are also available at the MACHO home page (http://wwwmacho.mcmaster.ca/). (c) 1997 American Astronomical Society.
- ID:
- ivo://CDS.VizieR/J/AJ/116/917
- Title:
- Micrometer measures of double stars
- Short Name:
- J/AJ/116/917
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Micrometer measures of 795 double stars made with the 26 inch (0.66m) refractor of the US Naval Observatory from 1984 to 1990 are presented.
- ID:
- ivo://CDS.VizieR/J/AJ/154/273
- Title:
- New orbits for 18 binaries
- Short Name:
- J/AJ/154/273
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Orbital elements of 18 visual binaries are computed using the measurements collected in the Fourth Catalog of Interferometric Measurements of Binary Stars; 15 orbits are determined for the first time and three orbits are revised. Eleven of the binaries, denoted as HDS, were discovered during the Hipparcos mission. The remaining binaries were discovered a few years earlier or later than 1991. All studied pairs are close, and all measured separations are less than 0.46". The shortest orbital period is 10 years and the longest orbital period is 127 years. Dynamical parallaxes and total masses of systems are derived from the orbital elements. We also give absolute magnitudes, spectral types, and (O-C) residuals in {theta} and {rho}.
- ID:
- ivo://CDS.VizieR/J/PAZh/24/343
- Title:
- New spectroscopic components
- Short Name:
- J/PAZh/24/343
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Based on the correlation radial-velocity measurement, we discovered new spectroscopic subsystems in the components of six visual multiple stars and determined the elements of their spectroscopic orbits.
- ID:
- ivo://CDS.VizieR/J/AJ/117/2980
- Title:
- NIR photometric studies of R Canis Majoris
- Short Name:
- J/AJ/117/2980
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present here the first light curves of the peculiar Algol binary system R Canis Majoris obtained in the near-infrared photometric bands J and K. The light curves are fitted for a semidetached model with the Wilson-Devinney light-curve synthesis program. Five epochs of primary minima and four epochs of secondary minima are obtained in the present study. The increased depth of the secondary minima in the near-IR bands compared with the optical bands enabled us to determine the moments of secondary minima with nearly the same accuracy as those of primary minima. All the secondary minima appear at phase 0.5, and the durations are equal for the primary and the secondary eclipses. The epochs of primary minima follow the nearly sinusoidal O-C curve that has been observed for this star in previous studies. The values of O-C for the secondary minima were in the same range as those of the primary minima observed by us.
- ID:
- ivo://CDS.VizieR/J/ApJ/844/103
- Title:
- Orbit alignment in triple stars
- Short Name:
- J/ApJ/844/103
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The statistics of the angle {Phi} between orbital angular momenta in hierarchical triple systems with known inner visual or astrometric orbits are studied. A correlation between apparent revolution directions proves the partial orbit alignment known from earlier works. The alignment is strong in triples with outer projected separation less than ~50au, where the average {Phi} is about 20{deg}. In contrast, outer orbits wider than 1000 au are not aligned with the inner orbits. It is established that the orbit alignment decreases with the increasing mass of the primary component. The average eccentricity of inner orbits in well-aligned triples is smaller than in randomly aligned ones. These findings highlight the role of dissipative interactions with gas in defining the orbital architecture of low-mass triple systems. On the other hand, chaotic dynamics apparently played a role in shaping more massive hierarchies. The analysis of projected configurations and triples with known inner and outer orbits indicates that the distribution of {Phi} is likely bimodal, where 80% of triples have {Phi}<70{deg} and the remaining ones are randomly aligned.
- ID:
- ivo://CDS.VizieR/J/MNRAS/422/2765
- Title:
- Orbital motion monitoring of A-star multiples
- Short Name:
- J/MNRAS/422/2765
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- As a part of our ongoing Volume-limited A-Star (VAST) adaptive optics survey, we have obtained observations of 26 binary systems with projected separations <100AU, 13 of which have sufficient historical measurements to allow for refinement of their orbital elements. For each system with an estimated orbit, the dynamical system mass obtained was compared with the system mass estimated from mass-magnitude relations. Discrepancies between the dynamical and theoretical system mass can be explained by the presence of a previously unresolved spectroscopic component, or by a non-solar metallicity of the system. Using this approach to infer the presence of additional companions, a lower limit to the fraction of binaries, triples, and quadruples can be estimated as 39%, 46%, and 15%, for systems with at least one companion within 100AU. The fraction of multiple systems with three or more components shows a relative increase compared to the fraction for Solar-type primaries resolved in previous volume-limited surveys. The observations have also revealed a pair of potentially young (<100Myr) M-dwarf companions, which would make an ideal benchmark for the theoretical models during the pre-Main Sequence contraction phase for M-dwarfs. In addition to those systems with orbit fits, we report 13 systems for which further orbital monitoring observations, are required, 11 of which are newly resolved as a part of the VAST survey.
- ID:
- ivo://CDS.VizieR/J/AJ/154/110
- Title:
- Orbits based on SOAR speckle interferometry. II.
- Short Name:
- J/AJ/154/110
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Orbits of 44 close and fast visual binaries are computed using the latest speckle observations; 23 orbits are determined for the first time, and the rest are revisions, some of those substantial. Six combined orbits use radial velocities. The median period is 15.6 years, and the shortest period is one year. Most stars are nearby late-type dwarfs. Dynamical parallaxes and estimates of the masses are derived from the orbital elements and the photometry of the components.
- ID:
- ivo://CDS.VizieR/J/AJ/152/138
- Title:
- Orbits based on speckle interferometry at SOAR
- Short Name:
- J/AJ/152/138
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The orbits of 55 visual binary stars are computed using recent speckle interferometry data from the SOAR telescope: 33 first-time orbits and 22 revisions of previous orbit calculations. The orbital periods range from 1.4-370 years, and the quality of the orbits ranges from definitive to preliminary and tentative. Most binaries consist of low-mass dwarfs and have short periods (median period 31 years). The dynamical parallaxes and masses are evaluated and compared to the Hipparcos parallaxes. Using differential speckle photometry, binary components are placed on the color-magnitude diagram.
