Apsidal Motion in Double Stars. I. Catalog

Петрова, А. В.; Орлов, В. В.

doi:10.1086/300671

Cited by 66 publications

(46 citation statements)

References 140 publications

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“…The first one is for example, by Hegedüs (1988), later updated by Petrova & Orlov (1999), while the most recent compilation of those stars is presented in Bulut & Demircan (2007). Their catalogue contains a total of 108 systems with known eccentricities and apsidal motion periods.…”

Section: Resultsmentioning

confidence: 99%

The first study of 54 new eccentric eclipsing binaries in our Galaxy

Zasche

Wolf

Uhlàř³

et al. 2018

A&A

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We present an analysis of the apsidal motion and light curve parameters of 54 never-before-studied galactic Algol-type binaries. This is the first analysis of such a large sample of eccentric eclipsing binaries in our Galaxy, and has enabled us to identify several systems that are worthy of further study. Bringing together data from various databases and surveys, supplemented with new observations, we have been able to trace the long-term evolution of the eccentric orbit over durations extending back up to several decades. Our present study explores a rather different sample of stars to those presented in the previously published catalogue of eccentric eclipsing binaries, sampling to fainter magnitudes, covering later spectral types, sensitive to different orbital periods with more than 50% of our systems having periods longer than six days. The typical apsidal motion in the sample is rather slow (mostly of order of centuries long), although in some cases this is less than 50 years. All of the systems, except one, have eccentricities less than 0.5, with an average value of 0.23. Several of the stars also show evidence for additional period variability. In particular we can identify three systems in the sample, HD 44093, V611 Pup, and HD 313631, which likely represent relativistic apsidal rotators.

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Section: Resultsmentioning

confidence: 99%

The first study of 54 new eccentric eclipsing binaries in our Galaxy

Zasche

Wolf

Uhlàř³

et al. 2018

A&A

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“…The lack of systems with shorter U can be understood as we selected only the DEBs. In DEBs the tidal effects are not as strong as in the systems with closer components for which U is sometimes very short (Petrova & Orlov 1999).…”

Section: Systems With Apsidal Motionmentioning

confidence: 97%

Detached binaries in the Large Magellanic Cloud

Michalska

Pigulski

2004

New Astronomy Reviews

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Abstract.As a result of a careful selection of eclipsing binaries in the Large Magellanic Cloud using the OGLE-II photometric database, we present a list of 98 systems that are suitable targets for spectroscopic observations that would lead to the accurate determination of the distance to the LMC. For these systems we derive preliminary parameters combining the OGLE-II data with the photometry of MACHO and EROS surveys. In the selected sample, 58 stars have eccentric orbits. Among these stars we found fourteen systems showing apsidal motion. The data do not cover the whole apsidal motion cycle, but follow-up observations will allow detailed studies of these interesting objects.

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“…significant one (see Table 11); the apsidal motion of the ninth system was arbitrarily fixed to a value close to the theoretical expectation. Interestingly, the system 5 266131 has a very fast apsidal motion, and probably holds the record among those hosting non-degenerate components (Petrova & Orlov 1999;Bulut & Demircan 2007). Note also that in two of these systems (5 123390 and 5 266131), the relative radius of the primary component is very close to, or even slightly exceeds, the limiting radius above which orbital circularization occurs quickly (North & Zahn 2003: they have r p = 0.238 and 0.281 respectively, while the limiting radius is ∼0.25.…”

Section: Apsidal Motionmentioning

confidence: 99%

VLT multi-object spectroscopy of 33 eclipsing binaries in the Small Magellanic Cloud

North¹,

Gauderon²,

Barblan

et al. 2010

A&A

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Aims. Our purpose is to provide reliable stellar parameters for a significant sample of eclipsing binaries, which are representative of a whole dwarf and metal-poor galaxy. We also aim at providing a new estimate of the mean distance to the SMC and of its depth along the line of sight for the observed field of view. Methods. We use radial velocity curves obtained with the ESO FLAMES facility at the VLT and light curves from the OGLE-II photometric survey. The radial velocities were obtained by least-squares fits of the observed spectra to synthetic ones, excluding the hydrogen Balmer lines. Results. Our sample contains 23 detached, 9 semi-detached and 1 overcontact systems. Most detached systems have properties consistent with stellar evolution calculations from single-star models at the standard SMC metalicity Z = 0.004, though they tend to be slightly overluminous. The few exceptions are probably due to third-light contribution or insufficient signal-to-noise ratio. The mass ratios are consistent with a flat distribution, both for detached and semi-detached/contact binaries. A mass-luminosity relation valid from ∼4 to ∼18 M is derived. The uncertainties are in the ±2 to ±11% range for the masses, in the ±2 to ±5% range for the radii and in the ±1 to ±6% range for the effective temperatures. The average distance modulus is 19.11 ± 0.03 (66.4 ± 0.9 kpc). The moduli derived from the V and from the I data are consistent within 0.01 mag. The 2σ depth of the SMC is, for our field, of 0.25 mag or 7.6 kpc under the assumption of a Gaussian distribution of stars along the line of sight. Three systems show significant apsidal motion, one of them with an apsidal period of 7.6 years, the shortest known to date for a detached system with main sequence stars.

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Apsidal Motion in Double Stars. I. Catalog

Cited by 66 publications

References 140 publications

The first study of 54 new eccentric eclipsing binaries in our Galaxy

The first study of 54 new eccentric eclipsing binaries in our Galaxy

Detached binaries in the Large Magellanic Cloud

VLT multi-object spectroscopy of 33 eclipsing binaries in the Small Magellanic Cloud

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