Apsidal motion and absolute parameters for five LMC eccentric eclipsing binaries

Zasche, P.; Wolf, M.

doi:10.1051/0004-6361/201322054

Cited by 14 publications

(7 citation statements)

References 42 publications

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“…All these systems are early-type objects, exhibit an apsidal motion, and was only poorly studied until now. Similar studies of LMC EEBs have been presented by Michalska & Pigulski (2005), by Michalska (2007), by Zasche & Wolf (2013), and recently also by Hong et al (2014). A set of such binaries with known apsidal motion is still rather limited outside of our Galaxy, hence a new contribution to the topic is still very important.…”

Section: Introductionsupporting

confidence: 85%

Apsidal Motion and a Light Curve Solution for 13 LMC Eccentric Eclipsing Binaries

Zasche¹,

Wolf²,

Vraštil³

et al. 2015

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New CCD observations for thirteen eccentric eclipsing binaries from the Large Magellanic Cloud were carried out using the Danish 1.54-meter telescope located at the La Silla Observatory in Chile. These systems were observed for their times of minima and 56 new minima were obtained. These are needed for accurate determination of the apsidal motion. Besides that, in total 436 times of minima were derived from the photometric databases OGLE and MACHO. The O − C diagrams of minima timings for these B-type binaries were analysed and the parameters of the apsidal motion were computed. The light curves of these systems were fitted using the program PHOEBE, giving the light curve parameters. We derived for the first time the relatively short periods of the apsidal motion ranging from 21 to 107 years. The system OGLE-LMC-ECL-07902 was also analysed using the spectra and radial velocities, resulting in masses 6.8, and 4.4 M ⊙ for the eclipsing components. For one system (OGLE-LMC-ECL-20112), the third-body hypothesis was also used for describing the residuals after subtraction of the apsidal motion, resulting in period of about 22 years. For several systems an additional third light was also detected, which makes these systems suspicious of triplicity.

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Section: Introductionsupporting

confidence: 85%

Apsidal Motion and a Light Curve Solution for 13 LMC Eccentric Eclipsing Binaries

Zasche¹,

Wolf²,

Vraštil³

et al. 2015

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“…All the timings were fitted to Eq. (1) by using the code (available at http://sirrah.troja.mff.cuni.cz/~zasche/ Programs.html) given by Zasche et al (2009) and Zasche & Wolf (2013). We made small corrections of the code by considering the inclination of the eclipsing pair in it and involving up to sixth power of the eccentricity.…”

Section: Discussion Of Apsidal Motion Periodmentioning

confidence: 99%

Apsidal Motion Study of Close Binary System CW Cephei

Han¹,

Jeong²,

Yoon³

et al. 2015

Journal of Astronomy and Space Sciences

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New observations for the times of minimum lights of a well-known apsidal motion star CW Cephei were made using a 0.6 m wide field telescope at Jincheon station of Chungbuk National University Observatory, Korea during the 2015 observational season. We determined new times of minimum lights from these observations and analyzed O-C diagrams together with collected times of minima to study both the apsidal motion and the Light Time Effect (LTE) suggested in the system. The new periods of the apsidal motion and the LTE were calculated as 46.6 and 39.3 years, respectively, which were similar but improved accuracy than earlier ones investigated by Han et al. (2002), Erdem et al. (2004 and Wolf et al. (2006).

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“…This was a subject of several studies during the last couple of years. We have already published a series of papers on apsidal motion in SMC and LMC: Zasche & Wolf (2013), Zasche et al (2014), and Zasche et al (2015). And besides that, the apsidal motion was studied by other authors, most recently (and also most comprehensively) by Hong et al (2016) presenting altogether 90 systems with apsidal motion in SMC, and Hong et al (2015) studying 27 SMC systems.…”

Section: Introductionmentioning

confidence: 99%

Apsidal Motion and Absolute Parameters of 21 Early-type Small Magellanic Cloud Eccentric Eclipsing Binaries

Zasche¹,

Wolf²

2019

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We present the apsidal motion as well as the light curve analyses of 21 eccentric eclipsing binaries located in the Small Magellanic Cloud. Most of these systems have never been studied before, hence their orbital and physical properties as well as the apsidal motion parameters are given here for the first time. All the systems are of early spectral type, having the orbital periods up to 4 days. The apsidal motion periods were derived to be from 7.2 to 200 years (OGLE-SMC-ECL-2194 having the shortest apsidal period among known main sequence systems). The orbital eccentricities are usually rather mild (median of about 0.06), maximum eccentricity being 0.33. For the period analysis using the O−C diagrams of eclipse timings, in total 951 minima were derived from survey photometry as well as our new data. Moreover, 6 systems show some additional variation in their O − C diagrams, which should indicate the presence of hidden additional components in them. According to our analysis these third-body variations have periods from 6.9 to 22 years.

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Apsidal motion and absolute parameters for five LMC eccentric eclipsing binaries

Cited by 14 publications

References 42 publications

Apsidal Motion and a Light Curve Solution for 13 LMC Eccentric Eclipsing Binaries

Apsidal Motion and a Light Curve Solution for 13 LMC Eccentric Eclipsing Binaries

Apsidal Motion Study of Close Binary System CW Cephei

Apsidal Motion and Absolute Parameters of 21 Early-type Small Magellanic Cloud Eccentric Eclipsing Binaries

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