V456 Ophiuchi and V490 Cygni: Systems with the shortest apsidal-motion periods

Zasche, P.; Wolf, M.

doi:10.1051/0004-6361/201015720

Cited by 3 publications

(2 citation statements)

References 19 publications

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“…Moreover, the classical MLR and MRR have been proven to be useful and are widely applied. For example, the MLR and MRR of Malkov (2007) has been used by Catanzaro & Ripepi (2014), Fumel & Böhm, (2012), Ripepi et al (2011), and Zasche & Wolf (2011). The MLR and MRR of Demircan & Kahraman (1991) were used by Jiang et al (2009), Kraus et al (2009), Hunter et al (2008), and Li et al (2005).…”

Section: Introductionmentioning

confidence: 99%

Main-Sequence Effective Temperatures From a Revised Mass–luminosity Relation Based on Accurate Properties

et al. 2015

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The mass-luminosity (M − L), mass-radius (M − R) and mass-effective temperature (M − T ef f ) diagrams for a subset of galactic nearby main-sequence stars with masses and radii accurate to ≤ 3% and luminosities accurate to ≤ 30% (268 stars) has led to a putative discovery. Four distinct mass domains have been identified, which we have tentatively associated with low, intermediate, high, and very high mass main-sequence stars, but which nevertheless are clearly separated by three distinct break points at 1.05, 2.4, and 7M ⊙ within the mass range studied of 0.38 − 32M ⊙ . Further, a revised mass-luminosity relation (MLR) is found based on linear fits for each of the mass domains identified. The revised, mass-domain based MLRs, which are classical (L ∝ M α ), are shown to be preferable to a single linear, quadratic or cubic equation representing as an alternative MLR. Stellar radius evolution within the main-sequence for stars with M > 1M ⊙ is clearly evident on the M − R diagram, but it is not the clear on the M − T ef f diagram based on published temperatures. Effective temperatures can be calculated directly using the well-known Stephan-Boltzmann law by employing the accurately known values of M and R with the newly defined MLRs. With the calculated temperatures, stellar temperature evolution within the main-sequence for stars with M > 1M ⊙ is clearly visible on the M − T ef f diagram.Our study asserts that it is now possible to compute the effective temperature of a mainsequence star with an accuracy of ∼ 6%, as long as its observed radius error is adequately small (< 1%) and its observed mass error is reasonably small (< 6%).A calibration sample was formed by selecting main-sequence stars with the most accurate masses, radii and effective temperatures from Table 2 of "The Catalogue of Stellar Parameters ..." by Eker et al. (2014), which is already reprocessed and homogenized. In the first step, our preliminary criteria involved finding stars where both mass and radius with errors of less than or equal to 3%, and luminosities with errors less than or equal to 30% were available. Among 514 stars (257 binaries), 296 stars were found fulfilling the criteria.In the second step, 25 stars outside of the main sequence were removed.The process of removing non-main-sequence stars was completed by using the mass-radius diagram. Compared to effective temperatures and luminosities, which can only be inferred indirectly, masses and radii provide much more reliable indicators of stellar properties, and a highly improved diagnostic tool for analyzing stellar evolution. Fig. 1 shows 271 main-sequence stars selected for the calibration sample and 25 non main-sequence stars on the M − R diagram. Theoretical ZAMS (Zero Age Main Sequence) and TAMS (Terminal Age Main Sequence) lines for metallicity zero from Bertelli et al. (2008Bertelli et al. ( , 2009 were used as border lines to secure the stars within the main-sequence band.Although metallicity data is missing in the catalogue of Eker et al. (2014), the thin-disk field stars in ...

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Section: Introductionmentioning

confidence: 99%

Main-Sequence Effective Temperatures From a Revised Mass–luminosity Relation Based on Accurate Properties

et al. 2015

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“…Among other stars (in addition to OGLE LMC-ECL-17226), additional systems having a very rapid apsidal motion of about ten years or even faster were also found: OGLE LMC-ECL-06837 (U = 9.9 yr), #17774 (U = 7.2 yr), -22613 (U = 6.6 yr), -23298 (U = 12.2 yr), -25047 (U = 10.8 yr). To date, the system with the fastest apsidal advance in our Galaxy is V490 Cyg (Zasche, & Wolf 2011) having U = 18.6 yr, while out of our Galaxy, it is the star from the SMC named OGLE SMC-ECL-2194 having U = 7.1 yr (Hong et al 2015). For the list of all our analysed systems and their results, see Tables A.3 and A.4.…”

Section: Resultsmentioning

confidence: 99%

First apsidal motion and light curve analysis of 162 eccentric eclipsing binaries from LMC

Zasche

Wolf

Kučáková

et al. 2020

A&A

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We present an extensive study of 162 early-type binary systems located in the LMC galaxy that show apsidal motion and have never been studied before. For the ample systems, we performed light curve and apsidal motion modelling for the first time. These systems have a median orbital period of 2.2 days and typical periods of the apsidal motion were derived to be of the order of decades. We identified two record-breaking systems. The first, OGLE LMC-ECL-22613, shows the shortest known apsidal motion period among systems with main sequence components (6.6 years); it contains a third component with an orbital period of 23 years. The second, OGLE LMC-ECL-17226, is an eccentric system with the shortest known orbital period (0.9879 days) and with quite fast apsidal motion period (11 years). Among the studied systems, 36 new triple-star candidates were identified based on the additional period variations. This represents more than 20% of all studied systems, which is in agreement with the statistics of multiples in our Galaxy. However, the fraction should only be considered as a lower limit of these early-type stars in the LMC because of our method of detection, data coverage, and limited precision of individual times of eclipses.

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A Comprehensive Catalog of Galactic Eclipsing Binary Stars with Eccentric Orbits Based on Eclipse Timing Diagrams

Kim

Kreiner

Zakrzewski

et al. 2018

ApJS

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V456 Ophiuchi and V490 Cygni: Systems with the shortest apsidal-motion periods

Cited by 3 publications

References 19 publications

Main-Sequence Effective Temperatures From a Revised Mass–luminosity Relation Based on Accurate Properties

Main-Sequence Effective Temperatures From a Revised Mass–luminosity Relation Based on Accurate Properties

First apsidal motion and light curve analysis of 162 eccentric eclipsing binaries from LMC

A Comprehensive Catalog of Galactic Eclipsing Binary Stars with Eccentric Orbits Based on Eclipse Timing Diagrams

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