Eclipsing binary statistics – Theory and observation

Söderhjelm, S.; Dischler, Johann

doi:10.1051/0004-6361:20042541

Cited by 15 publications

(29 citation statements)

References 18 publications

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“…The Hipparcos data were obtained as the mean value of Figs. 14 and 15 in Söderhjelm & Dischler (2005).…”

Section: Discussionmentioning

confidence: 97%

“…Evaluating the capability of ground-based surveys this way has the advantage that it includes not only the photometric precision of the data in the evaluation but also the phase coverage and the detection algorithms. Figure 8 shows the number of eclipsing binaries in the BEST data compared with the Hipparcos data (Söderhjelm & Dischler 2005). A description of how the eclipsing binaries are detected in the Hipparcos data can be found in Söderhjelm & Dischler (2005).…”

Section: Data Completenessmentioning

confidence: 99%

“…Figure 8 shows the number of eclipsing binaries in the BEST data compared with the Hipparcos data (Söderhjelm & Dischler 2005). A description of how the eclipsing binaries are detected in the Hipparcos data can be found in Söderhjelm & Dischler (2005). The Hipparcos stars have been separated into two different We have tried to compare the BEST data with the Hipparcos data from both bins with more or less the same result, although the close Hipparcos sample seems to fit the BEST data slightly better than the distant sample.…”

Section: Data Completenessmentioning

confidence: 99%

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Identification of Variable Stars inCOROT's First Main Observing Field (LRc1)

et al. 2007

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The COROT space mission will monitor several target fields for up to 150 days to perform asteroseismology and to search for extrasolar planets by photometric transits. Variable stars in the target fields are important objects for additional scientific studies but can also disturb the search for planetary transits. A variability characterization of the target fields prior to COROT observations is therefore important for two reasons: to find interesting variable stars to monitor further and to make an analysis of the impact of the variable stars on detecting extrasolar planet transits with COROT. The Berlin Exoplanet Search Telescope ( BEST ) is a small wide-angle telescope dedicated to highprecision photometry. It has observed a 9 deg 2 field of view centered at ( ; ) ¼ (19 h 00 m 00:0 s ; þ00 01 0 55:2 00 ) (J2000.0) over 98 nights to search for variable stars in the surroundings of the first long-run target field ( LRc1) of the COROT space mission. In this data set we identified 92 periodic variable stars, 86 of which are new discoveries and 6 of which are known from the General Catalogue of Variable Stars (GCVS). For five of the GCVS stars, variability could not be confirmed. Forty-three of the 92 detected periodic variable stars are identified as eclipsing binaries. We have evaluated the completeness of our survey for eclipsing binaries by comparing it to the expected fraction of eclipsing binaries based on Hipparcos observations. From this evaluation we show that the BEST data set presented here has a completeness of 20%Y30% for periods longer than 1 day and is complete relative to Hipparcos for short-period binaries.

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“…The Hipparcos data were obtained as the mean value of Figs. 14 and 15 in Söderhjelm & Dischler (2005).…”

Section: Discussionmentioning

confidence: 97%

Section: Data Completenessmentioning

confidence: 99%

Section: Data Completenessmentioning

confidence: 99%

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Identification of Variable Stars inCOROT's First Main Observing Field (LRc1)

et al. 2007

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“…Figure 8 also shows that there is a tendency for OBSG systems to have longer periods. This might be attributed in part to the larger size of the components (Söderhjelm & Dischler 2005).…”

Section: Ob Supergiants Starsmentioning

confidence: 99%

A systematic study of variability among OB-stars based on HIPPARCOS photometry

Lefèvre

Марченко²,

Moffat

et al. 2009

A&A

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Context. Variability is a key factor for understanding the nature of the most massive stars, the OB stars. Such stars lie closest to the unstable upper limit of star formation. Aims. In terms of statistics, the data from the HIPPARCOS satellite are unique because of time coverage and uniformity. They are ideal to study variability in this large, uniform sample of OB stars. Methods. We used statistical techniques to determine an independant threshold of variability corresponding to our sample of OB stars, and then applied an automatic algorithm to search for periods in the data of stars that are located above this threshold. We separated the sample stars into 4 main categories of variability: 3 intrinsic and 1 extrinsic. The intrinsic categories are: OB main sequence stars (∼2/3 of the sample), OBe stars (∼10%) and OB Supergiant stars (∼1/4).The extrinsic category refers to eclipsing binaries. Results. We classified about 30% of the whole sample as variable, although the fraction depends on magnitude level due to instrumental limitations. OBe stars tend to be much more variable (≈80%) than the average sample star, while OBMS stars are below average and OBSG stars are average. Types of variables include α Cyg, β Cep, slowly pulsating stars and other types from the general catalog of variable stars. As for eclipsing binaries, there are relatively more contact than detached systems among the OBMS and OBe stars, and about equal numbers among OBSG stars.

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“…However, the recent paper by Söderhjelm & Dischler (2005) shows how one might proceed in estimating ψ(q). They have developed a population synthesis code that predicts the properties of eB's as a function of eclipse depth and orbital period.…”

Section: Eclipse-probability Biasmentioning

confidence: 99%

Spectroscopic binaries with components of similar mass

Lucy

2006

A&A

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The assertion that there is an intrinsic excess of binaries with mass ratios q 1 -the twin hypothesis -is investigated. A strong version of this hypothesis (H s ), due to Lucy & Ricco (1979, AJ, 84, 401) and Tokovinin (2000, A&A, 360, 997), refers to a narrow peak in the distribution function ψ(q) for q > ∼ 0.95. A weak version (H w ), due to Halbwachs et al. (2003, A&A, 397, 159), refers to a broad peak for q > ∼ 0.8. Current data on SB2's is analysed and H s is found to be statistically significant for a sample restricted to orbits of high precision. But claims that H s is significant for binaries with special characteristics are not confirmed since the sample sizes are well below the minimum required for a reliable test. With regard to H w , additional observational evidence is not presented, but evidence to the contrary in the form of Hogeveen's (1992, Ap&SS, 196, 299) model of biased sampling with ψ ∝ q −2 is criticized. Specifically, his success in thus fitting catalogued data depends on implausible assumptions about the research methodologies of binary-star spectroscopists.

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Eclipsing binary statistics – Theory and observation

Cited by 15 publications

References 18 publications

Identification of Variable Stars inCOROT's First Main Observing Field (LRc1)

Identification of Variable Stars inCOROT's First Main Observing Field (LRc1)

A systematic study of variability among OB-stars based on HIPPARCOS photometry

Spectroscopic binaries with components of similar mass

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